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The article presents some aspects of the implementation of regional policy in order to enhance the development of regions through the formation of strategies as tools for strategic management of the region. Special emphasis is placed on the specifics of strategic planning of tourism development in a regional context, which is based on a strategic analysis of the current socio-economic situation of the region using social and economic evaluation criteria. The groups are identified and the characteristics of the economic development indicators of the regions are given, the specific characteristics inherent in regional tourism in the context of its strategic planning process are determined. All of the above processes create a new configuration of the spatial development of the country, through the formation of zones of advanced economic growth, including using the sectoral specialization of the regions. At the same time, the competitive advantage of the regions of the South of Russia is determined by the tourist vector of their development as the most promising. The article describes the cycle of strategic planning of regional tourism development, which includes a number of stages: determining the goals of tourism development in the region; analysis of the external and internal environment of the development of the region; development of a concept and development strategy; development of an industry development plan; analysis of efficiency and effectiveness, adjustment of goals and methods to achieve them. The approaches to strategic planning of the development of socio-economic objects from foreign practice are presented, based on a system of indicators that allow an objective assessment of the development of its potential, which are understood as a set of characteristics formalizing the description of the main parameters that provide the choice of the optimal variant of the system functioning at different stages of the strategy implementation. In addition, the normative legal acts of various levels regulating modern socio-economic relations in the tourism sector of the regions are given; macro and micro tools for the development of regional tourism on the example of the Republic of Crimea are defined.

Relevance. The conceptual task of epidemiological surveillance as part of the sanitary protection of the territory of the Russian Federation (RF) from the importation and spread of diseases that pose a danger to the population at the present stage is to identify potential risks of a sanitary and еpidemic emergency and prompt response if they occur. Epidemic manifestations of diseases caused by new respiratory viruses, in most cases, cause a crisis in public health, which indicates the need for a comprehensive study of the features of their course, determination of criteria for the potential risk of an emergency of an еpidemic nature, which will make it possible to timely organize a complex of anti-epidemic (preventive) measures. Aim. Study, systematize and stratify the features of the atypical course of the epidemic process of acute respiratory viral infections caused by new variants of the pathogen in a city with a population of more than one million people. Materials and methods. The study used retrospective data on infectious morbidity in different age groups from government reports for the period 2015–2020, data from annual forms No. 2 of the federal state statistical observation for the period 2009–2020. Rospotrebnadzor Administration for the Rostov Region, Center for Hygiene and Epidemiology in the Rostov Region. Statistical data processing was carried out by a generally accepted method. Results. The analysis showed that the periods 2009–2010, 2015–2016, 2020–2021 had significant changes in the epidemic process in relation to its typical long-term course with a predominance in the structure of the incidence of ARVI, including influenza and new coronavirus infection, of various age groups for each period, an atypically severe infectious process and an increase in the number of community-acquired pneumonia. Moreover, in the periods 2009–2010, 2015–2016. Influenza A (H1N1) pdm09 virus was dominant in the etiological structure, in 2020–2021 – the causative agent of the new coronavirus infection SARS-CoV-2. ...

We present RadioAstron Space VLBI imaging observations of the BL Lac object S5 0716+71 made on 2015 January 3-4 at a frequency of 22 GHz (wavelength λ = 1.3 cm). The observations were made in the framework of the AGN Polarization Key Science Program. The source was detected on projected space-ground baselines up to 70,833 km (5.6 Earth diameters) for both parallel-hand and cross-hand interferometric visibilities. We have used these detections to obtain a full-polarimetric image of the blazar at an unprecedented angular resolution of 24 μas, the highest for this source to date. This enabled us to estimate the size of the radio core to be 2.2 × 1013 K for the blazar core. This implies that the inverse-Compton limit must be violated in the rest frame of the source, even for the largest Doppler factor δ ∼ 25 reported for 0716+714. © 2020. The American Astronomical Society. All rights reserved. ; We thank the anonymous referee for useful comments which helped to improve the manuscript. The authors are grateful to Uwe Bach for providing measurements of the absolute EVPA orientation obtained at Effelsberg. E.V.K. acknowledges support from the Italian Space Agency under contract ASIINAF 2015-023-R.O. J.L.G. and A.F. were supported by the Spanish Ministry of Economy and Competitiveness grants AYA2013-40825-P and AYA2016-80889-P. Y.Y.K. was supported by the government of the Russian Federation (agreement 05.Y09.21.0018) and the Alexander von Humboldt Foundation. G.B. acknowledges financial support under the INTEGRAL ASI-INAF agreement 2013-025.R01. The RadioAstron project is led by the Astro Space Center of the Lebedev Physical Institute of the Russian Academy of Sciences and the Lavochkin Scientific and Production Association under a contract with the State Space Corporation ROSCOSMOS, in collaboration with partner organizations in Russia and other countries. Results of optical positioning measurements of the Spektr-R spacecraft by the global MASTER Robotic Net (Lipunov et al. 2010), ISON collaboration, and Kourovka observatory were used for spacecraft orbit determination in addition to mission facilities. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2018). This study makes use of 43 GHz VLBA data from the VLBA-BU Blazar Monitoring Program (VLBA-BU-BLAZAR), funded by NASA through the Fermi Guest Investigator grants, the most recent 80NSSC17K0649. The VLBA is an instrument of the Long Baseline Observatory. The Long Baseline Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by the Aalto University. This work is partly based on observations carried out using the 100 m telescope of the MPIfR (MaxPlanck-Institute for Radio Astronomy) at Effelsberg, the Noto telescope operated by INAF—Istituto di Radioastronomia and the 32 m radio telescope operated by Torun Centre for Astronomy of Nicolaus Copernicus University in Torun (Poland) and supported by the Polish Ministry of Science and Higher Education SpUB grant. The European VLBI Network is a joint facility of independent European, African, Asian, and North American radio astronomy institutes. Scientific results from data presented in this publication are derived from the following global VLBI project code: GL041. Facilities: RadioAstron Space Radio Telescope (Spektr-R), VLBA, Green Bank 100 m radio telescope, Sheshan 25 m radio telescope (Shangai), EVN, Effelsberg 100 m radio telescope, Noto 32 m radio telescope. Software: AIPS (Greisen 2003), Difmap (Pearson et al. 1994), ROOT framework (Antcheva et al. 2009). ; Peer reviewed

This article examines the key stages of the evolution of spiritual and moral education based on Orthodox Christian values, starting from the early days of Christianity and ending with the present period, when the Church becomes one of the most important institutions influencing the formation of spiritual and moral qualities of young people. The purpose of the research is to study the fundamental foundations of spiritual and moral Christian teaching, their reflection in the historiosophy of the Orthodox religion. and their significance in the formation of a person's worldview of the present time. The conclusions drawn in the course of the study allow us to reliably assert that the spiritual and moral values of Orthodoxy are natural and organic to the Russian mental character in any period of its development. That is why, in the XXI century, a return to traditional values by redirecting education and upbringing as mutually dependent sides of a single process into a spiritual and moral traditional path will allow the Russian people to find their own path in world history.

The paper examines the role of international historians within the Soviet peacekeeping movement from the sec-ond half of the 1950s to the 1980s, with a particular focus on the Pugwash Conferences on Science and World Af-fairs. By analyzing published materials and archival documents from the Archive of the Russian Academy of Scienc-es, the study explores the intellectual contributions of international historians to the organizational, rhetorical, and ideological aspects of the peacekeeping movement formation. The authors focuses on prominent figures, such as V.M. Khvostov, a historian of diplomacy, V.G. Trukhanovsky, a British Studies scholar, E.M. Primakov, an expert in Arab Studies, G.A. Arbatov, an Americanist, A.N. Glinkin, a specialist in the Latin American Studies, and A.M. Vasiliev and V.B. Kokorev, Africanists. The research challenges the notion that historical symbols played a signifi-cant role in Soviet peacekeeping rhetoric, highlighting instead that international historians primarily acted as analysts of contemporary international relations, rarely drawing on the past as a symbolic resource. The figure of an interna-tional historian performing a diplomatic mission reflects the specifics of the Soviet disciplinary structure, where in-ternational relations have been integrated into historical disciplines since the time of Stalin. Khvostov personified this tradition. The authors trace the evolution of themes discussed at the Pugwash conferences and how Soviet representa-tion within these conferences changed depending on this. While the early conferences focused on the threat of nucle-ar war and the prospects for disarmament, the range of topics expanded noticeably in subsequent years. For example, since the mid-1970s, African problems have gained increasing prominence in the activities of the Pugwash move-ment, requiring the involvement of relevant specialists. The paper demonstrates the evolution of Soviet analytics of international relations presented at the Pugwash conferences, transitioning from ideologized techniques and analyti-cal structures in the spirit of the 1940s to a more modern and pragmatic approach. This shift indicates an increasing level of expertise among Soviet historians of international relations.

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.-- Open Access funding provided by Max Planck Society. ; Context Detailed studies of relativistic jets in active galactic nuclei (AGN) require high-fidelity imaging at the highest possible resolution. This can be achieved using very long baseline interferometry (VLBI) at radio frequencies, combining worldwide (global) VLBI arrays of radio telescopes with a space-borne antenna on board a satellite. Aims. We present multiwavelength images made of the radio emission in the powerful quasar S5 0836+710, obtained using a global VLBI array and the antenna Spektr-R of the RadioAstron mission of the Russian Space Agency, with the goal of studying the internal structure and physics of the relativistic jet in this object. Methods. The RadioAstron observations at wavelengths of 18 cm, 6 cm, and 1.3 cm are part of the Key Science Program for imaging radio emission in strong AGN. The internal structure of the jet is studied by analyzing transverse intensity profiles and modeling the structural patterns developing in the flow. Results. The RadioAstron images reveal a wealth of structural detail in the jet of S5 0836+710 on angular scales ranging from 0.02 mas to 200 mas. Brightness temperatures in excess of 1013 K are measured in the jet, requiring Doppler factors of 100 for reconciling them with the inverse Compton limit. Several oscillatory patterns are identified in the ridge line of the jet and can be explained in terms of the Kelvin Helmholtz (KH) instability. The oscillatory patterns are interpreted as the surface and body wavelengths of the helical mode of the KH instability. The interpretation provides estimates of the jet Mach number and of the ratio of the jet to the ambient density, which are found to be Mj 12 and 0:33. The ratio of the jet to the ambient density should be conservatively considered an upper limit because its estimate relies on approximations. © L. Vega-García et al. 2020 ; L.V.G. is a member of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. The RadioAstron project is led by the Astro Space Center of the Lebedev Physical Institute of the Russian Academy of Sciences and the Lavochkin Scientific and Production Association under a contract with the State Space Corporation ROSCOSMOS, in collaboration with partner organizations in Russia and other countries. This research is based on observations correlated at the Bonn Correlator, jointly operated by the Max Planck Institute for Radio Astronomy (MPIfR), and the Federal Agency for Cartography and Geodesy (BKG). The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Thanks to Phillip Edwards and Alan Roy for the useful comments about the paper. M.P. has been supported by the Spanish Ministerio de Economia y Competitividad (grants AYA2015-66899-C2-1-P and AYA2016-77237-C3-3-P) and the Generalitat Valenciana (grant PROMETEOII/2014/069). This work was partially supported by the COST Action MP0904 Black Holes in a Violent Universe. G.B. acknowledges financial support under the INTEGRAL ASI-INAF agreement 2013-025-R.1. T.S. was supported by the Academy of Finland projects 274477, 284495, and 312496. I.A. acknowledges support by a Ramon y Cajal grant of the Ministerio de Economia, Industria y Competitividad (MINECO) of Spain. The research at the IAA-CSIC was partly supported by the MINECO through grants AYA2016-80889-P, AYA2013-40825-P, and AYA2010-14844. Y.Y.K. was supported in part by the government of the Russian Federation (agreement 05.Y09.21.0018) and the Alexander von Humboldt Foundation. ; Peer reviewed

We present Space-VLBI RadioAstron observations at 1.6 GHz and 4.8 GHz of the flat spectrum radio quasar 3C 273, with detections on baselines up to 4.5 and 3.3 Earth Diameters, respectively. Achieving the best angular resolution at 1.6 GHz to date, we have imaged limb-brightening in the jet, not previously detected in this source. In contrast, at 4.8 GHz, we detected emission from a central stream of plasma, with a spatial distribution complementary to the limb-brightened emission, indicating an origin in the spine of the jet. While a stratification across the jet width in the flow density, internal energy, magnetic field, or bulk flow velocity are usually invoked to explain the limb-brightening, the different jet structure detected at the two frequencies probably requires a stratification in the emitting electron energy distribution. Future dedicated numerical simulations will allow the determination of which combination of physical parameters are needed to reproduce the spine-sheath structure observed by Space-VLBI with RadioAstron in 3C 273. © ESO 2021. ; JLG and AF acknowledge financial support from the Spanish Ministerio de Economia y Competitividad (grants AYA2016-80889-P, PID2019-108995GB-C21), the Consejeria de Economia, Conocimiento, Empresas y Universidad of the Junta de Andalucia (grant P18-FR-1769), the Consejo Superior de Investigaciones Cientificas (grant 2019AEP112), and the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). APL, YYK, and ABP were supported by the Russian Science Foundation (project 20-62-46021). TS was partly supported by the Academy of Finland projects 274477 and 315721. MP acknowledges the support by the Spanish Ministerio de Ciencia e Innovacion (MICINN) under grant PID2019-105510GB-C31. MP and JMM acknowledge financial support from the Spanish Ministry of Science through Grants PID2019-107427GB-C33 and AYA2016-77237-C3-3-P, and from the Generalitat Valenciana through grant PROMETEU/2019/071. JMA was supported by the German Research Foundation grant HE5937/2-2. LIG acknowledges support by the CSIRO Distinguished Visitor Programme. The RadioAstron project is led by the Astro Space Center of the Lebedev Physical Institute of the Russian Academy of Sciences and the Lavochkin Scientific and Production Association under a contract with the Roscosmos State Corporation, in collaboration with partner organizations in Russia and other countries. This publication has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No. 730562 [RadioNet]. ; Peer reviewed

Nonlinear optics is an increasingly important field for scientific and technological applications, owing to its relevance and potential for optical and optoelectronic technologies. Currently, there is an active search for suitable nonlinear material systems with efficient conversion and a small material footprint. Ideally, the material system should allow for chip integration and room-temperature operation. Two-dimensional materials are highly interesting in this regard. Particularly promising is graphene, which has demonstrated an exceptionally large nonlinearity in the terahertz regime. Yet, the light–matter interaction length in two-dimensional materials is inherently minimal, thus limiting the overall nonlinear optical conversion efficiency. Here, we overcome this challenge using a metamaterial platform that combines graphene with a photonic grating structure providing field enhancement. We measure terahertz third-harmonic generation in this metamaterial and obtain an effective third-order nonlinear susceptibility with a magnitude as large as 3 × 10–8 m2/V2, or 21 esu, for a fundamental frequency of 0.7 THz. This nonlinearity is 50 times larger than what we obtain for graphene without grating. Such an enhancement corresponds to a third-harmonic signal with an intensity that is 3 orders of magnitude larger due to the grating. Moreover, we demonstrate a field conversion efficiency for the third harmonic of up to ∼1% using a moderate field strength of ∼30 kV/cm. Finally, we show that harmonics beyond the third are enhanced even more strongly, allowing us to observe signatures of up to the ninth harmonic. Grating-graphene metamaterials thus constitute an outstanding platform for commercially viable, CMOS-compatible, room-temperature, chip-integrated, THz nonlinear conversion applications. ; K.-J.T. acknowledges funding from the European Union's Horizon 2020 research and innovation program under Grant Agreement No. 804349 (ERC StG CUHL) and financial support through the MAINZ Visiting Professorship. ICN2 was supported by the Severo Ochoa program from Spanish MINECO Grant No. SEV-2017-0706. Parts of this research were carried out at ELBE at the Helmholtz-Zentrum Dresden-Rossendorf e.V., a member of the Helmholtz Association. N.A., S.K., and I.I. acknowledge support from the European Union's Horizon 2020 research and innovation program under Grant Agreement No. 737038 (TRANSPIRE). X.J. acknowledges the support from the Max Planck Graduate Center with the Johannes Gutenberg-Universität Mainz (MPGC). ; Peer reviewed

Funding Information: We thank the anonymous referee for useful comments. JLG and AF acknowledge financial support from the Spanish Ministerio de Economia y Competitividad (grants AYA2016-80889-P, PID2019-108995GBC21), the Consejeria de Economia, Conocimiento, Empresas y Universidad of the Junta de Andalucia (grant P18-FR-1769), the Consejo Superior de Investigaciones Cientificas (grant 2019AEP112), and the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). APL, YYK, and ABP were supported by the Russian Science Foundation (project 20-62-46021). TS was partly supported by the Academy of Finland projects 274477 and 315721. MP acknowledges the support by the Spanish Ministerio de Ciencia e Innovacion (MICINN) under grant PID2019-105510GB-C31. MP and JMM acknowledge financial support from the Spanish Ministry of Science through Grants PID2019-107427GB-C33 and AYA2016-77237-C3-3-P, and from the Generalitat Valenciana through grant PROMETEU/2019/071. JMA was supported by the German Research Foundation grant HE5937/2-2. LIG acknowledges support by the CSIRO Distinguished Visitor Programme. Funding Information: Acknowledgements. We thank the anonymous referee for useful comments. JLG and AF acknowledge financial support from the Spanish Ministerio de Economía y Competitividad (grants AYA2016-80889-P, PID2019-108995GB-C21), the Consejería de Economía, Conocimiento, Empresas y Universidad of the Junta de Andalucía (grant P18-FR-1769), the Consejo Superior de Investi-gaciones Científicas (grant 2019AEP112), and the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). APL, YYK, and ABP were supported by the Russian Science Foundation (project 20-62-46021). TS was partly supported by the Academy of Finland projects 274477 and 315721. MP acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31. MP and JMM acknowledge financial support from the Spanish Ministry of Science through Grants PID2019-107427GB-C33 and AYA2016-77237-C3-3-P, and from the Generali-tat Valenciana through grant PROMETEU/2019/071. JMA was supported by the German Research Foundation grant HE5937/2-2. LIG acknowledges support by the CSIRO Distinguished Visitor Programme. The RadioAstron project is led by the Astro Space Center of the Lebedev Physical Institute of the Russian Academy of Sciences and the Lavochkin Scientific and Production Association under a contract with the Roscosmos State Corporation, in collaboration with partner organizations in Russia and other countries. This publication has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No. 730562 [RadioNet]. This paper includes data observed with the 100-m Effelsberg radio-telescope, which is operated by the Max-Planck-Institut für Radioastronomie in Bonn (Germany). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The European VLBI Network is a joint facility of independent European, African, Asian, and North American radio astronomy institutes. The Long Baseline Array is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO. This research made use of Python (http://www.python.org), Numpy (van der Walt et al. 2011), Pandas (McKinney 2010), and Matplotlib (Hunter 2007). We also made use of Astropy Publisher Copyright: © ESO 2021. ; We present Space-VLBI RadioAstron observations at 1.6 GHz and 4.8 GHz of the flat spectrum radio quasar 3C 273, with detections on baselines up to 4.5 and 3.3 Earth Diameters, respectively. Achieving the best angular resolution at 1.6 GHz to date, we have imaged limb-brightening in the jet, not previously detected in this source. In contrast, at 4.8 GHz, we detected emission from a central stream of plasma, with a spatial distribution complementary to the limb-brightened emission, indicating an origin in the spine of the jet. While a stratification across the jet width in the flow density, internal energy, magnetic field, or bulk flow velocity are usually invoked to explain the limb-brightening, the different jet structure detected at the two frequencies probably requires a stratification in the emitting electron energy distribution. Future dedicated numerical simulations will allow the determination of which combination of physical parameters are needed to reproduce the spine-sheath structure observed by Space-VLBI with RadioAstron in 3C 273. ; Peer reviewed

RadioAstron is a 10 m orbiting radio telescope mounted on the Spektr-R satellite, launched in 2011, performing Space Very Long Baseline Interferometry (SVLBI) observations supported by a global ground array of radio telescopes. With an apogee of ∼350 000 km, it is offering for the first time the possibility to perform μas-resolution imaging in the cm-band. Aims. The RadioAstron active galactic nuclei (AGN) polarization Key Science Project (KSP) aims at exploiting the unprecedented angular resolution provided by RadioAstron to study jet launching/collimation and magnetic-field configuration in AGN jets. The targets of our KSP are some of the most powerful blazars in the sky. Methods. We present observations at 22 GHz of 3C 273, performed in 2014, designed to reach a maximum baseline of approximately nine Earth diameters. Reaching an angular resolution of 0.3 mas, we study a particularly low-activity state of the source, and estimate the nuclear region brightness temperature, comparing with the extreme one detected one year before during the RadioAstron early science period. We also make use of the VLBA-BU-BLAZAR survey data, at 43 GHz, to study the kinematics of the jet in a ∼1.5-yr time window. Results. We find that the nuclear brightness temperature is two orders of magnitude lower than the exceptionally high value detected in 2013 with RadioAstron at the same frequency (1.4 × 10 13 K, source-frame), and even one order of magnitude lower than the equipartition value. The kinematics analysis at 43 GHz shows that a new component was ejected ∼2 months after the 2013 epoch, visible also in our 22 GHz map presented here. Consequently this was located upstream of the core during the brightness temperature peak. Fermi-LAT observations for the period 2010â '2014 do not show any Î 3-ray flare in conjunction with the passage of the new component by the core at 43 GHz. Conclusions. These observations confirm that the previously detected extreme brightness temperature in 3C 273, exceeding the inverse Compton limit, is a short-lived phenomenon caused by a temporary departure from equipartition. Thus, the availability of interferometric baselines capable of providing μas angular resolution does not systematically imply measured brightness temperatures over the known physical limits for astrophysical sources.© 2017 ESO. ; Scientific results from data presented in this publication are derived from the EVN project code GA030C (ground array), and from the RadioAstron mission project code RAKS04C (space segment). J.L.G. and A.F. acknowledge support by the Spanish Ministry of Economy and Competitiveness grants AYA2013-40825-P and AYA2016-80889-P. A. A. and M.A.P.T. acknowledge support by the Spanish MINECO through grants AYA2012-38491-C02-02 and AYA2015-63939-C2-1-P, cofunded with FEDER funds. E.R. acknowledges support from the Spanish MINECO through grants AYA2012-38491-C02-01 and AYA2015-63939-C2-2-P and from the Generalitat Valenciana grant PROMETEOII/2014/057. T.S. was funded by the Academy of Finland projects 274477 and 284495. The research at Boston University was supported in part by NASA Fermi Guest Investigator grant NNX14AQ58G. S.S.L. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIP) (No. NRF-2016R1C1B2006697). Y. Y. K. was supported in part by the Alexander von Humboldt Foundation. This research has made use of data from the OVRO 40-m monitoring program (Richards et al. 2011) which is supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G and NSF grants AST-0808050 and AST-1109911. ; Peer Reviewed