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Kosugi, K. Matsuzaki, T. Sakao, et al., Solar Phys. 243, 3 (2007).",{"doi":211},"10.1007\u002Fs11207-007-9014-6",{"id":20,"text":213,"url":20,"identifiers":214},"B. Lites, H. Socas-Navarro, M. Kubo, et al., Publ. Astron. Soc. Japan 59, 571 (2007).",{"doi":215},"10.1093\u002Fpasj\u002F59.sp3.S571",{"id":20,"text":217,"url":20,"identifiers":218},"B. Lites, M. Kubo, H. Socas-Navarro, et al., Astrophys. J. 460, 1237 (2008).",{"doi":219},"10.1086\u002F522922",{"id":20,"text":221,"url":20,"identifiers":222},"B. Lites, K. D. Leka, A. Skumanich, et al., Astrophys. J. 460, 1019 (1996).",{"doi":223},"10.1086\u002F177028",{"id":20,"text":225,"url":20,"identifiers":226},"N. Meunier, S. K. Solanki, and W. C. Livingston, Astron. Astrophys. 331, 771 (1998).",{},{"id":20,"text":228,"url":20,"identifiers":229},"B. Lites, A. Skumanich, and V. Martinez Pillet, Astron. Astrophys. 333, 1053 (1998).",{},{"id":20,"text":231,"url":20,"identifiers":232},"B. De Pontieu, Astrophys. J. 569, 474 (2002).",{"doi":233},"10.1086\u002F339231",{"id":20,"text":235,"url":20,"identifiers":236},"M. J. Martinez González, M. Collados, B. Ruiz Cobo, and S. K. Solanki, Astron. Astrophys. 469, L39 (2007).",{"doi":237},"10.1051\u002F0004-6361:20077505",{"id":20,"text":239,"url":20,"identifiers":240},"R. Centeno, H. Socas-Navarro, B. Lites, et al., Astrophys. J. 666, L137 (2007).",{"doi":241},"10.1086\u002F521726",{"id":20,"text":243,"url":20,"identifiers":244},"D. Orozco Suárez, L. R. Bellot Rubio, J. C. del Toro Iniesta, et al., Astrophys. J. 670, L61 (2007).",{"doi":245},"10.1086\u002F524139",{"id":20,"text":247,"url":20,"identifiers":248},"J. W. Harvey, D. Branston, C. J. Henney, and C. U. Keller, Astrophys. J. 659, L177 (2007).",{"doi":249},"10.1086\u002F518036",{"id":20,"text":251,"url":20,"identifiers":252},"R. Ishikawa, S. Tsuneta, K. Ichimoto, et al., Astron. Astrophys. 481, L25 (2008).",{"doi":253},"10.1051\u002F0004-6361:20079022",{"id":20,"text":255,"url":20,"identifiers":256},"U. Grossmann-Doerth, M. Schüssler, and O. Steiner, Astron. Astrophys. 337, 928 (1998).",{},{"id":20,"text":258,"url":20,"identifiers":259},"A. S. Gadun, V. A. Sheminova, and S. K. Solanki, Kinemat. Fiz. Nebesn. Tel 15(5), 387 (1999).",{},{"id":20,"text":261,"url":20,"identifiers":262},"A. S. Gadun, S. K. Solanki, V. A. Sheminova, and S. R. O. Ploner, Solar Phys. 203, 1 (2001).",{"doi":263},"10.1023\u002FA:1012729811113",{"id":20,"text":265,"url":20,"identifiers":266},"W. Schaffenberger, S. Wedemeyer-Bohm, O. Steiner, and B. Freytag, in Solar MHD Theory and Observations, Ed. by J. Leibacher, R. E. Stein, and H. Uitenbroek, ASP Conf. Ser. 354, 345 (2006).",{},{"id":20,"text":268,"url":20,"identifiers":269},"O. Steiner, R. Rezaei, W. Schaffenberger, and S. Wedemeyer-Bohm, Astrophys. J. 680, L85 (2008).",{"doi":270},"10.1086\u002F589740",{"id":20,"text":272,"url":20,"identifiers":273},"M. Schüssler and A. Vögler, Astron. Astrophys. 481, L5 (2008).",{"doi":274},"10.1051\u002F0004-6361:20078998",{"id":20,"text":276,"url":20,"identifiers":277},"O. Steiner, in Modern Solar Facilities-Advanced Solar Science, Ed. by F. Kneer, K. G. Puschmann, and A. D. Wittmann (Universitatsverlag, Göttingen, 2007).",{},{"id":20,"text":279,"url":20,"identifiers":280},"M. Asplund, H.-G. Ludwig, Å. Nordlund, and R. F. Stein, Astron. Astrophys. 359, 669 (2000).",{},{"id":20,"text":282,"url":20,"identifiers":283},"A. S. Gadun, S. K. Solanki, and A. Johannesson, Astron. Astrophys. 350, 1018 (1999).",{},{"id":20,"text":285,"url":20,"identifiers":286},"S. R. O. Ploner, S. K. Solanki, and A. S. Gadun, Astron. Astrophys. 352, 679 (1999).",{},{"id":20,"text":288,"url":20,"identifiers":289},"I. N. Atroshchenko and V. A. Sheminova, Kinemat. Fiz. Nebesn. Tel 12(4), 32 (1996).",{},{"id":20,"text":291,"url":20,"identifiers":292},"A. S. Gadun, Kinemat. Fiz. Nebesn. Tel 16(2), 99 (2000).",{},{"id":20,"text":294,"url":20,"identifiers":295},"V. A. Sheminova and A. S. Gadun, Astron. Zh. 77, 790 (2000) [Astron. Rep. 44, 701 (2000)].",{},{"id":20,"text":297,"url":20,"identifiers":298},"W. Deinzer, G. Hensler, M. Schüssler, and E. Weisshaar, Astron. Astrophys. 139, 435 (1984).",{},{"id":20,"text":300,"url":20,"identifiers":301},"P. N. Brandt and A. S. Gadun, Kinemat. Fiz. Nebesn. Tel 11(4), 44 (1995).",{},{"id":20,"text":303,"url":20,"identifiers":304},"S. R. O. Ploner, M. Schüssler, S. K. Solanki, and A. S. Gadun, in Advanced Solar Polarimetry—Theory, Observation, and Instrumentation, Ed. by M. Sigwarth, ASP Conf. Ser. 236, 363 (2001).",{},{"id":20,"text":306,"url":20,"identifiers":307},"R. F. Stein and Å. Nordlund, in IAU Colloquim 188: Magnetic Coupling of the Solar Atmosphere, Ed. by H. Sawaya-Lacoste (ESA Publ. Division, 2002), p. 83.",{},{"id":20,"text":309,"url":20,"identifiers":310},"L. R. Bellot Rubio, R. Luis, I. Rodrígues Hidalgo, et al., Astron. Astrophys. 560, 1010 (2001).",{},{"id":20,"text":312,"url":20,"identifiers":313},"S. R. O. Ploner, M. Schüssler, S. K. Solanki, et al., in Advanced Solar Polarimetry—Theory, Observation, and Instrumentation, Ed. by M. Sigwarth, ASP Conf. Ser. 236, 371 (2001).",{},{"id":20,"text":315,"url":20,"identifiers":316},"V. A. Sheminova, Kinemat. Fiz. Nebesn. Tel 21(3), 172 (2005) [Kinem. Phys. Celest. Bodies 21, 120 (2005)].",{},{"id":20,"text":318,"url":20,"identifiers":319},"V. A. Sheminova, Solar Phys. 254, 29 (2009).",{"doi":320},"10.1007\u002Fs11207-008-9286-5",{"id":20,"text":322,"url":20,"identifiers":323},"A. Vögler, S. Shelyag, M. Schüssler, et al., Astron. Astrophys. 429, 335 (2005).",{"doi":324},"10.1051\u002F0004-6361:20041507",{"id":20,"text":326,"url":20,"identifiers":327},"R. F. Stein and Å. Nordlund, Astrophys. J. 642, 1246 (2006).",{"doi":328},"10.1086\u002F501445",{"id":20,"text":330,"url":20,"identifiers":331},"B.W. Lites, Astrophys. J. 573, 431 (2002).",{"doi":332},"10.1086\u002F340120",{"id":20,"text":334,"url":20,"identifiers":335},"J. Sánchez Almeida, Astron. Astrophys. 450, 1198 (2006).",{"doi":336},"10.1051\u002F0004-6361:20054331",{"id":20,"text":338,"url":20,"identifiers":339},"I. Domínguez Cerdeña, J. Almeida Sánchez, and F. Kneer, Astrophys. J. 407, 741 (2003).",{},{"id":20,"text":341,"url":20,"identifiers":342},"P. S. Barklem, N. Piskunov, and B. J. O’Mara, Astron. Astrophys. Suppl. Ser. 142, 467 (2000).",{"doi":343},"10.1051\u002Faas:2000167",{"id":20,"text":345,"url":20,"identifiers":346},"V. A. Sheminova, Calculating the Profiles of Stokes Parameters of Magnetoactive Absorption Lines in Stellar Atmospheres, Dep. VINITI May 30, 1990, No. 2940-V90 (Kiev, Ukraina, 1990) [in Russian].",{},false,{"id":349,"createTime":350,"updateTime":351,"relativeEntities":352,"slug":353,"properties":354,"entityType":119,"verifyStatus":120,"verifyTime":365,"verifyNote":122,"languages":20,"translateLanguages":20,"viewCount":21,"primaryUrl":366,"fullTextUrl":20,"authors":367,"publicationType":146,"publisherRelationship":384,"citationCount":21,"citationInfo":436,"publishDate":439,"publishYear":437,"citationAnalyzeStatus":440,"lastCitationAnalyze":351,"indexDatabases":441,"openAccess":20,"references":20,"isForceReanalyzing":347},"a9dfedd4-8d3a-4d62-8150-0a7cde8b0108","2023-12-12T04:19:05.346+00:00","2026-07-29T09:45:26.074+00:00",[],"The-motion-of-a-globular-cluster-inside-a-rotating-layered-inhomogeneous-elliptical-galaxy",{"abstract":355,"title":357,"gsPaper":359,"references":361,"doi":363},{"EN":356},"We consider the spatial motion of a globular cluster with a constant or variable mass inside a rotating, layered, inhomogenous elliptical galaxy with a constant or variable mass. An analog to the Jacobi integral is found, regions of possiblemotion are determined, and zero-velocity surfaces constructed. Stationary solutions (libration points) are determined, together with their stability according to the Lyapunov criterion. In the case of variable mass, the autonomization method is used to solve the equations of motion, and the autonomization criteria used to establish an analog of the Eddington-Jeans law for the variation of the density of the galaxy.",{"EN":358},"The motion of a globular cluster inside a rotating, layered, inhomogeneous elliptical galaxy",{"VOID":360},"[\"3455538666719073424\"]",{"VOID":362},"L. R. Spitler, D. A. Forbes, J. Strader, et al., Mon. Not. R. Astron. Soc. 385, 361 (2008).\nL. P. Bassino, T. Richtler, and B. Dirsch, Mon.Not. R. Astron. Soc. 367, 156 (2006).\nN. Tamura, R. M. Sharples, N. Arimoto, et al., Mon. Not. R. Astron. Soc. 373, 588 (2006).\nK. L. Rhode and S. E. Zepf, Astron. J. 121, 210 (2001).\nP. Côté, D. E. McLaughlin, J. G. Cohen, et al., Astrophys. J. 591, 850 (2003).\nG. de Vaucouleurs, A. de Vaucouleurs, H. Corwin, et al., Third Reference Catalouge of Bright Galaxies, Vols. 2, 3 (Springer, New York, 1991).\nS. Chandrasekhar, Principles of Stellar Dynamics (Univ. Chicago, Chicago, 1942; Inostr. Liter., Moscow, 1948).\nS. A. Gasanov, Pis’ma Astron. Zh. 29, 792 (2003) [Astron. Lett. 29, 704 (2003)].\nG. N. Duboshin, Celestial Mechanics. Fundamental Problems and Methods (Nauka, Moscow, 1968) [in Russian].\nI. S. Gradshteyn and I. M. Ryzhik, Tables of Integrals, Series and Products (GIFML, Moscow, 1963; Academic, New York, 1980).\nF. Schweizer, in New Horizons in Globular Cluster Astronomy, Ed. by G. Piotto et al., ASP Conf. Ser. 296, 467 (2003).\nA. V. Kravtsov and O. Y. Gnedin, Astrophys. J. 623, 650 (2005).\nH. Poincaré, Lectures on Hypothesis of Cosmogony (Lib. Sci.A. Hermann et fills, Paris, 1911).\nB. P. Kondrat’ev, Potential Theory and Figures of Equilibrium (Inst. Komp. Issled., Moscow, Izhevsk, 2003) [in Russian].\nS. A. Gasanov and L. G. Luk’yanov, Astron. Zh. 79, 944 (2002) [Astron. Rep. 46, 851 (2002)].\nS. A. Gasanov, Pis’ma Astron. Zh. 32, 217 (2006) [Astron. Lett. 32, 192 (2006)].\nYu. V. Batrakov, Byull. In-ta Teor. Astron. 6, 524 (1957).\nV. K. Abalakin, Byull. In-ta Teor. Astron. 6, 543 (1957).\nS. G. Zhuravlev, Astron. Zh. 51, 1330 (1974) [Sov. Astron. 18, 792 (1974)].\nS. A. Gasanov, Pis’ma Astron. Zh. 27, 150 (2001) [Astron. Lett. 27, 124 (2001)]\nS. A. Gasanov, Pis’ma Astron. Zh. 33, 925 (2007) [Astron. Lett. 33, 827 (2007)].\nN. M. Matveev, Methods of Integration of Ordinary Differential Equations (Vyssh. Shkola, Moscow, 1967) [in Russian].\nS. A. Gasanov, Pis’ma Astron. Zh. 34, 202 (2008) [Astron. Lett. 34, 179 (2008)].\nS. A. Gasanov, Astron. Zh. 86, 826 (2009) [Astron. Rep. 53, 769 (2009)].\nI.W. Mestschersky, Astron. Nachr. 132, 129 (1893).\nI.W. Mestschersky, Astron. Nachr. 159, 229 (1902).\nB. E. Gel’fgat, Byull. In-ta Teor. Astron. 7, 354 (1959).\nL. G. Luk’yanov, Astron. Zh. 66, 385 (1989).\nJ. F. Navarro, C. S. Frenk, and S. D. M. White, Astrophys. J. 490, 493 (1997).\nG. Illingworth, Astrophys. J. 218, L43 (1977).",{"VOID":364},"10.1134\u002FS1063772910030029","2024-06-25T15:10:27.291+00:00","http:\u002F\u002Flink.springer.com\u002F10.1134\u002FS1063772910030029",[368],{"id":369,"sortIndex":21,"researcher":20,"roles":370,"affiliations":372,"properties":381,"displayName":383,"givenName":20,"familyName":20},"a56378cb-3b40-4d35-94b9-016478d4df7a",[371],"AUTHOR",[373],{"id":374,"sortIndex":21,"affiliation":375,"properties":20},"0a05db3f-e3ab-4f77-89f7-94f89e9d262d",{"id":374,"createTime":20,"updateTime":20,"relativeEntities":376,"slug":20,"properties":377,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":380,"statistic":20},[],{"title":378},{"VI":379},"Sternberg Astronomical Institute, Moscow State University, Moscow, Russia",[],{"title":382},{"VI":383},"S. A. 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Due to a large radial optical thickness, the equatorial regions of the disk are heated by infrared radiation from the disk surface (atmosphere), which in turn is heated by the direct radiation from the star. It was previously shown that interception of the stellar radiation by inhomogeneities on the disk surface can cause perturbations that propagate towards the star. In this work, within a detailed 1+1D-dimensional numerical model of a protoplanetary disk, the occurrence of such waves is studied. It was found that, in a disk that is optically thick to its own radiation, surface perturbations indeed form and propagate towards the star, which confirms the conclusions of other authors. However, in contrast to analytical predictions, we found that, for sufficiently massive disks, thermal waves affect only the upper layers without significant temperature fluctuations in the equatorial plane. The results obtained indicate the need to study this instability within more consistent hydrodynamic models.",{"EN":452},"Simulation of Thermal Surface Waves in a Protoplanetary Disk in 1+1D Approximation",{"VOID":454},"[\"14924519646766225571\"]",{"VOID":456},"10.1134\u002FS1063772922050055","2024-04-29T20:51:10.740+00:00","https:\u002F\u002Flink.springer.com\u002Farticle\u002F10.1134\u002FS1063772922050055",[460,475,488],{"id":461,"sortIndex":21,"researcher":20,"roles":462,"affiliations":463,"properties":472,"displayName":474,"givenName":20,"familyName":20},"ad0fae1b-ef5c-4281-8727-06d41e3b5373",[371],[464],{"id":465,"sortIndex":21,"affiliation":466,"properties":20},"17db2e80-e3bd-4ba2-b97a-b9bc2cce9a55",{"id":465,"createTime":20,"updateTime":20,"relativeEntities":467,"slug":20,"properties":468,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":471,"statistic":20},[],{"title":469},{"VI":470},"Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia",[],{"title":473},{"VI":474},"Ya. 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L. Brogan, L. M. Pérez, T. R. Hunter, W. R. F. Dent, et al., Astrophys. J. Lett. 808, L3 (2015); arXiv: 1503.02649 [astro-ph.SR].",{"arxiv":563},"arXiv:1503.02649",{"id":20,"text":565,"url":20,"identifiers":566},"S. M. Andrews, Ann. Rev. Astron. Astrophys. 58, 483 (2020); arXiv: 2001.05007 [astro-ph.EP].",{"arxiv":567},"arXiv:2001.05007",{"id":20,"text":569,"url":20,"identifiers":570},"J. Huang, S. M. Andrews, C. P. Dullemond, A. Isella, et al., Astrophys. J. Lett. 869, L42 (2018); arXiv: 1812.04041 [astro-ph.EP].",{"arxiv":571},"arXiv:1812.04041",{"id":20,"text":573,"url":20,"identifiers":574},"C. Baruteau, A. Crida, S. J. Paardekooper, F. Masset, et al., in Protostars and Planets VI, Ed. by H. Beuther, R. S. Klessen, C. P. Dullemond, and T. Henning (Univ. of Arizona Press, Tucson, 2014), p. 667; arXiv: 1312.4293 [astro-ph.EP].",{"arxiv":575},"arXiv:1312.4293",{"id":20,"text":577,"url":20,"identifiers":578},"R. Dong, Z. Zhu, and B. Whitney, Astrophys. J. 809, 93 (2015); arXiv: 1411.6063 [astro-ph.EP].",{"arxiv":579},"arXiv:1411.6063",{"id":20,"text":581,"url":20,"identifiers":582},"G. Dipierro, G. Laibe, D. J. Price, and G. Lodato, Mon. Not. R. Astron. Soc. 459, L1 (2016); arXiv: 1602.07457 [astro-ph.EP].",{"arxiv":583},"arXiv:1602.07457",{"id":20,"text":585,"url":20,"identifiers":586},"J. Bae, Z. Zhu, and L. Hartmann, Astrophys. J. 850, 201 (2017); arXiv: 1706.03066 [astro-ph.EP].",{"arxiv":587},"arXiv:1706.03066",{"id":20,"text":589,"url":20,"identifiers":590},"S. Zhang, Z. Zhu, J. Huang, V. V. Guzmán, et al., Astrophys. J. Lett. 869, L47 (2018); arXiv:1812.04045 [astro-ph.EP].",{"arxiv":591},"arXiv:1812.04045",{"id":20,"text":593,"url":20,"identifiers":594},"P. D’Alessio, J. Cantó, L. Hartmann, N. Calvet, and S. Lizano, Astrophys. J. 511, 896 (1999).",{},{"id":20,"text":596,"url":20,"identifiers":597},"C. P. Dullemond, Astron. Astrophys. 361, L17 (2000); arXiv: astro-ph\u002F0007399.",{"arxiv":598},"arXiv:astro-ph\u002F0007399",{"id":20,"text":600,"url":20,"identifiers":601},"S.-I. Watanabe and D. N. C. Lin, Astrophys. J. 672, 1183 (2008); arXiv: 0709.1760 [astro-ph].",{"arxiv":602},"arXiv:0709.1760",{"id":20,"text":604,"url":20,"identifiers":605},"R. Siebenmorgen and F. Heymann, Astron. Astrophys. 539, A20 (2012); arXiv: 1201.3577 [astro-ph.SR].",{"arxiv":606},"arXiv:1201.3577",{"id":20,"text":608,"url":20,"identifiers":609},"T. Ueda, M. Flock, and T. Birnstiel, Astrophys. J. Lett. 914, L38 (2021); arXiv: 2105.13852 [astro-ph.EP].",{"arxiv":610},"arXiv:2105.13852",{"id":20,"text":612,"url":20,"identifiers":613},"Y. Wu and Y. Lithwick, arXiv: 2105.02680 [astro-ph.EP] (2021).",{"arxiv":614},"arXiv:2105.02680",{"id":20,"text":616,"url":20,"identifiers":617},"E. I. Vorobyov and Y. N. Pavlyuchenkov, Astron. Astrophys. 606, A5 (2017); arXiv: 1706.00401 [astro-ph.GA].",{"arxiv":618},"arXiv:1706.00401",{"id":20,"text":620,"url":20,"identifiers":621},"Y. N. Pavlyuchenkov, A. V. Tutukov, L. A. Maksimova, and E. I. Vorobyov, Astron. Rep. 64, 1 (2020); arXiv: 1912.08572 [astro-ph.SR].",{"arxiv":622},"arXiv:1912.08572",{"id":20,"text":624,"url":20,"identifiers":625},"L. A. Maksimova, Y. N. Pavlyuchenkov, and A. V. Tutukov, Astron. Rep. 64, 815 (2020); arXiv: 2009.07750 [astro-ph.SR].",{"arxiv":626},"arXiv:2009.07750",{"id":20,"text":628,"url":20,"identifiers":629},"N. N. Kalitkin, Numerical Methods (Nauka, Moscow, 1978) [in Russian].",{},{"id":20,"text":631,"url":20,"identifiers":632},"A. N. Youdin and J. Goodman, Astrophys. J. 620, 459 (2005); arXiv: astro-ph\u002F0409263.",{"arxiv":633},"arXiv:astro-ph\u002F0409263",{"id":635,"createTime":636,"updateTime":637,"relativeEntities":638,"slug":639,"properties":640,"entityType":119,"verifyStatus":120,"verifyTime":651,"verifyNote":122,"languages":20,"translateLanguages":20,"viewCount":21,"primaryUrl":652,"fullTextUrl":20,"authors":653,"publicationType":146,"publisherRelationship":669,"citationCount":93,"citationInfo":721,"publishDate":724,"publishYear":722,"citationAnalyzeStatus":19,"lastCitationAnalyze":725,"indexDatabases":726,"openAccess":20,"references":20,"isForceReanalyzing":347},"58a0fc99-ed64-4cda-80bf-e1b2b348941f","2024-01-29T19:36:29.521+00:00","2026-07-23T16:22:50.206+00:00",[],"The-force-function-of-two-rigid-celestial-bodies-in-Delaunay-Andoyer-variables",{"abstract":641,"title":643,"gsPaper":645,"references":647,"doi":649},{"EN":642},"Two new expansions of the force function of two rigid celestial bodies of finite size and arbitrary shape are obtained in Delaunay–Andoyer variables with any degree of accuracy, in the form of a partial sum of an eight dimensional Fourier series. These expansions of the force function contain products of expressions for the momenta and Stokes constants in terms of sines and cosines, whose arguments are linear combinations of the Delaunay and Andoyer angular variables. These representations of the force function are compact and convenient for applications in various problems in celestial mechanics and astrodynamics.",{"EN":644},"The force function of two rigid celestial bodies in Delaunay–Andoyer variables",{"VOID":646},"[\"8853074056253107397\"]",{"VOID":648},"B. P. Kondrat’ev, Theory of Potential. NewMethods and Problems with Solutions (Mir, Moscow, 2007) [in Russian].\nH. Andoyer, Cours de Méchanique Céleste (Gauthier-Villars, Paris, 1923).\nG. N. Duboshin, Celestial Mechanics. Fundamental Problems and Methods (Nauka, Moscow, 1975) [in Russian].\nH. Kinoshita, Publ. Astron. Soc. Jpn. 24, 423 (1972).\nA. A. Zlenko, Kosm. Issled. 19, 688 (1981).\nA. A. Zlenko, Cand. Sci. (Phys. Math.) Dissertation (Sternberg Astron. Inst., Moscow State Univ., Moscow, 1982).\nA. A. Zlenko, Translational-Rotational Motion of Resonance Satellites (Inter. Academy of Information Technologies, Moscow, 2004) [in Russian].\nYu. G. Markov, Kosm. Issled. 26, 236 (1988).\nYu. V. Barkin, in Figure and Dynamics of the Earth, Moon and Planets, Proceedings of the International Symposium, Prague, Czechoslovakia, September 15–20, 1986, Ed. by P. Holota, Monogr. Ser. of UGTK (Res. Inst. of Geodesy, Topography and Cartography, Czechosl. Acad. Sci., Prague, 1987), p. 657.\nP. S. Krasil’nikov, Int. J. Non-Lin. Mech. 73, 43 (2015).\nM. Šidlichovský, Bull. Astron. Inst. Checosl. 29, 90 (1978).\nM. Šidlichovský, Bull. Astron. Inst. Checosl. 30, 152 (1979).\nM. Šidlichovský, Bull. Astron. Inst. Checosl. 32, 159 (1981).\nE. P. Aksenov and V. V. Chazov, The Model of Earth Artificial Satellite Motion. Main Problem, Basic Algorithms (Gos. Astron. Inst. Shternberga, Mosk. Gos. 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Twelve objects with redshifts from 0.573 to 2.694 have been classiffied as quasars, and two objects with featureless spectra as BL Lac objects. Four objects are emission-line radio galaxies with redshifts from 0.204 to 0.311 (one also displaying absorption lines), and one object is an absorption-line galaxy with a redshift of 0.214. Radio flux densities have been obtained at six frequencies for all the sources except for two extended objects. The radio spectra of five of the sources can be separated into extended and compact components. Three objects display substantial rapid (on time scales from several days to several weeks) and long-term variability of their flux densities.",{"EN":992},"Spectral studies with the Special Astrophysical Observatory 6 m and RATAN-600 telescopes",{"VOID":994},"[\"18109185361525034353\"]",{"VOID":996},"P. C. Gregory, W. K. Scott, K. Douglas, and J. J. Condon, Astrophys. J., Suppl. Ser. 103, 427 (1996).\nA. G. Gorshkov, V. K. Konnikova, and M. G. Mingaliev, Astron. Zh. 80, 978 (2003) [Astron. Rep. 47, 903 (2003)].\nM. P. Veron-Cetty and P. Veron, Astron. Astrophys. 374, 92 (2001).\nV. Chavushyan, R. Mujica, J. R. Valdez, et al., Astron. Zh. 79, 771 (2002) [Astron. Rep. 46, 697 (2002)].\nV. L. Afanas’ev, S. N. Dodonov, A. V. Moiseev, et al., Pis’ma Astron. Zh. 29, 626 (2003) [Astron. Lett. 29, 579 (2003)].\nhttp:\u002F\u002Fwww.sao.ru\u002Fmoisav\u002Fscorpio\u002Fscorpio.html.\nA. M. Botashev, A. G. Gorshkov, V. K. Konnikova, and M. G. Mingaliev, Astron. Zh. 76, 723 (1999) [Astron. Rep. 43, 631 (1999)].\nA. G. Gorshkov and O. I. Khromov, Astrofiz. Issled., Izv. Spets. Astrofiz. Obs. 14, 15 (1981).\nI. W. A. Browne, Mon. Not. R. Astron. Soc. 293, 257 (1998).\nJ. J. Condon, W. D. Cotton, E. W. Greisen, et al., Astron. J. 115, 1693 (1998).\nJ. N. Douglas, Astron. J. 111, 1945 (1996).\nD. Monet, A. Bird, B. Canzian, et al., USNO-SA1.0 (US Naval Observatory, Washington DC, 1996).\nA. P. Marscher and W. K. Gear, Astrophys. J. 298, 114 (1985).\nE. Valtaoja, H. Terasranta, S. Urpo, et al., Astron. Astrophys. 254, 71 (1992).\nJ. H. Simmonetti, J. M. Cordes, and D. S. Heeschen, Astrophys. J. 296, 46 (1985).\nP. A. Hughes, H. D. Aller, and V. F. Aller, Astrophys. 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Moiseev",{"VOID":1044},"[\"tSdlPxMAAAAJ\"]",{"id":1046,"sortIndex":94,"researcher":20,"roles":1047,"affiliations":1048,"properties":1057,"displayName":1059,"givenName":20,"familyName":20},"770b89e6-3376-4adc-9e2e-460489c869d4",[371],[1049],{"id":1050,"sortIndex":21,"affiliation":1051,"properties":20},"b2fc732e-25e6-4f88-8373-3daaa74ed61d",{"id":1050,"createTime":20,"updateTime":20,"relativeEntities":1052,"slug":20,"properties":1053,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1056,"statistic":20},[],{"title":1054},{"VI":1055},"Sternberg Astronomical Institute, Moscow, Russia",[],{"title":1058},{"VI":1059},"A. G. Gorshkov",{"id":1061,"sortIndex":93,"researcher":20,"roles":1062,"affiliations":1063,"properties":1070,"displayName":1072,"givenName":20,"familyName":20},"029bc7dd-29d7-443b-8868-4315d93a754c",[371],[1064],{"id":1050,"sortIndex":21,"affiliation":1065,"properties":20},{"id":1050,"createTime":20,"updateTime":20,"relativeEntities":1066,"slug":20,"properties":1067,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1069,"statistic":20},[],{"title":1068},{"VI":1055},[],{"title":1071},{"VI":1072},"V. K. Konnikova",{"id":1074,"sortIndex":835,"researcher":20,"roles":1075,"affiliations":1076,"properties":1083,"displayName":1085,"givenName":20,"familyName":20},"6ec53cc1-c805-4bf9-854b-3629381b289f",[371],[1077],{"id":1007,"sortIndex":21,"affiliation":1078,"properties":20},{"id":1007,"createTime":20,"updateTime":20,"relativeEntities":1079,"slug":20,"properties":1080,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1082,"statistic":20},[],{"title":1081},{"VI":1012},[],{"title":1084},{"VI":1085},"M. G. Mingaliev",{"url":1000,"publisher":1087,"properties":1133},{"id":6,"createTime":7,"updateTime":8,"relativeEntities":1088,"slug":10,"properties":1089,"entityType":18,"verifyStatus":19,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":21,"subjectFields":1093,"manageAffiliations":1102,"indexDatabases":1113,"url":86,"thumbnailPath":20,"statistic":1128,"gsStatistic":20,"type":97,"analyzePriority":20},[],{"issn":1090,"title":1091,"eissn":1092},{"VOID":13},{"EN":15},{"VOID":17},[1094,1098],{"id":24,"createTime":20,"updateTime":20,"relativeEntities":1095,"label":1096,"description":1097,"parentId":20,"standard":20,"scholarHubFieldId":20},[],{"EN":27},{},{"id":30,"createTime":20,"updateTime":20,"relativeEntities":1099,"label":1100,"description":1101,"parentId":20,"standard":20,"scholarHubFieldId":20},[],{"EN":33},{},[1103,1108],{"id":37,"createTime":20,"updateTime":20,"relativeEntities":1104,"slug":20,"properties":1105,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1107,"statistic":20},[],{"title":1106},{"EN":41},[],{"id":44,"createTime":20,"updateTime":20,"relativeEntities":1109,"slug":20,"properties":1110,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1112,"statistic":20},[],{"title":1111},{"EN":48},[],[1114,1121],{"id":52,"indexDatabase":1115,"url":63,"indexYears":64,"academicFieldIds":1120,"indexDatabaseRanking":68},{"id":54,"createTime":20,"updateTime":20,"relativeEntities":1116,"label":1117,"description":1118,"key":60,"publicationTags":1119,"standard":20},[],{"EN":57,"VI":57},{"EN":57,"VI":59},[62],[66,67],{"id":70,"indexDatabase":1122,"url":83,"indexYears":20,"academicFieldIds":1127,"indexDatabaseRanking":20},{"id":72,"createTime":20,"updateTime":20,"relativeEntities":1123,"label":1124,"description":1125,"key":79,"publicationTags":1126,"standard":20},[],{"EN":75,"VI":75},{"EN":77,"VI":78},[81,82],[85],{"impactFactor":21,"impactFactorByYear":1129,"i10Index":21,"i10IndexLast5Year":21,"totalPublication":89,"totalPublicationByYear":1130,"totalCitation":21,"totalCitationByYear":1131,"totalCitationPerPublication":21,"totalCitationPerPublicationByYear":1132,"hindexLast5Year":21,"hindex":21},{},{"2001":91,"2003":91,"2004":91,"2005":92,"2006":91,"2007":93,"2008":94,"2009":91,"2010":92,"2011":91,"2012":91,"2015":92,"2017":92,"2018":94,"2019":91,"2020":91,"2022":92,"2023":94},{},{},{"pages":1134,"volume":1136},{"VOID":1135},"374-389",{"VOID":1137},"49",8,{"total":1138,"publishYear":1140,"statisticByYear":1141},2005,{"2006":91,"2013":91,"2014":92,"2015":91,"2016":92,"2021":91},"2005-05-01","2026-07-19T17:24:25.234+00:00",[68,81],{"id":1146,"createTime":1147,"updateTime":1148,"relativeEntities":1149,"slug":1150,"properties":1151,"entityType":119,"verifyStatus":120,"verifyTime":1162,"verifyNote":122,"languages":20,"translateLanguages":20,"viewCount":21,"primaryUrl":1163,"fullTextUrl":20,"authors":1164,"publicationType":146,"publisherRelationship":1193,"citationCount":21,"citationInfo":1245,"publishDate":1248,"publishYear":1246,"citationAnalyzeStatus":440,"lastCitationAnalyze":1249,"indexDatabases":1250,"openAccess":20,"references":20,"isForceReanalyzing":347},"50dae0a6-bdfa-4907-8118-3adfd4634665","2023-12-07T18:56:51.093+00:00","2026-07-18T11:55:05.954+00:00",[],"Effect-of-coulomb-losses-on-the-spectra-of-heavy-particles-accelerated-in-prolonged-solar-events",{"abstract":1152,"title":1154,"gsPaper":1156,"references":1158,"doi":1160},{"EN":1153},"This paper examines the possibility of using the energy spectra of accelerated solar cosmic-ray ions and features formed by Coulomb losses to study the solar plasma (the power-law index S for the scattering turbulence, particle number density N, and temperature T of the background medium). For an individual solar flare, Coulomb losses can be manifest to different degrees in the spectra of different ions, providing a means to determine S. A comparison of theoretical spectra for H, He, C, O, and Fe ions with observed spectra for the prolonged solar flare of October 20, 1995 yields S≈3, N≈5×109 cm−3, and T≈106 K, assuming that the characteristic time scale over which these particles gain energy is about a second.",{"EN":1155},"Effect of coulomb losses on the spectra of heavy particles accelerated in prolonged solar events",{"VOID":1157},"[\"7194365198017150524\"]",{"VOID":1159},"H. V. Cane, R. E. McGuire, and T. T. von Rosenvinge, Astrophys. J. 301, 448 (1986).\nM. A. Lee and J. M. Ryan, Astrophys. J. 303, 829 (1986).\nS. V. Bulanov and P. V. Sasorov, Astron. Zh. 52, 763 (1975) [Sov. Astron. 19, 464 (1975)].\nYu. E. Litvinenko and B. V. Somov, Sol. Phys. 158, 317 (1995).\nM. Temerin and I. Roth, Astrophys. J. Lett. 391, L105 (1992).\nG. E. Kocharov, Itogi Nauki Tekh., Ser. 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Res. 102, 14631 (1997).\nR. Schlickeiser and J. Steinacker, Sol. Phys. 122, 29 (1989).\nR. Vainio and R. Schlickeiser, Astron. Astrophys. 331, 793 (1998).\nR. Vainio and R. Schlickeiser, Astron. Astrophys. 343, 303 (1999).\nA. Kruger, Introduction to Solar Radio Astronomy and Radio Physics (Reidel, Dordrecht, 1979; Mir, Moscow, 1984).\nS. Tsuneta, Astrophys. J. 456, 840 (1996).",{"VOID":1161},"10.1134\u002F1.1327642","2024-06-23T19:05:53.847+00:00","http:\u002F\u002Flink.springer.com\u002F10.1134\u002F1.1327642",[1165,1180],{"id":1166,"sortIndex":21,"researcher":20,"roles":1167,"affiliations":1168,"properties":1177,"displayName":1179,"givenName":20,"familyName":20},"6e8ca6a7-dc59-4d86-b7d3-744b00e16dd2",[371],[1169],{"id":1170,"sortIndex":21,"affiliation":1171,"properties":20},"0a6a6c8f-a5e0-42f3-b8f2-7638d5196cf8",{"id":1170,"createTime":20,"updateTime":20,"relativeEntities":1172,"slug":20,"properties":1173,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1176,"statistic":20},[],{"title":1174},{"VI":1175},"St. Petersburg State Technical University, St. Petersburg, Russia",[],{"title":1178},{"VI":1179},"M. F. Stovpyuk",{"id":1181,"sortIndex":91,"researcher":20,"roles":1182,"affiliations":1183,"properties":1190,"displayName":1192,"givenName":20,"familyName":20},"34bacc20-dd2d-41c1-b317-83611dcd89b0",[371],[1184],{"id":1170,"sortIndex":21,"affiliation":1185,"properties":20},{"id":1170,"createTime":20,"updateTime":20,"relativeEntities":1186,"slug":20,"properties":1187,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1189,"statistic":20},[],{"title":1188},{"VI":1175},[],{"title":1191},{"VI":1192},"V. M. Ostryakov",{"url":1163,"publisher":1194,"properties":1240},{"id":6,"createTime":7,"updateTime":8,"relativeEntities":1195,"slug":10,"properties":1196,"entityType":18,"verifyStatus":19,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":21,"subjectFields":1200,"manageAffiliations":1209,"indexDatabases":1220,"url":86,"thumbnailPath":20,"statistic":1235,"gsStatistic":20,"type":97,"analyzePriority":20},[],{"issn":1197,"title":1198,"eissn":1199},{"VOID":13},{"EN":15},{"VOID":17},[1201,1205],{"id":24,"createTime":20,"updateTime":20,"relativeEntities":1202,"label":1203,"description":1204,"parentId":20,"standard":20,"scholarHubFieldId":20},[],{"EN":27},{},{"id":30,"createTime":20,"updateTime":20,"relativeEntities":1206,"label":1207,"description":1208,"parentId":20,"standard":20,"scholarHubFieldId":20},[],{"EN":33},{},[1210,1215],{"id":37,"createTime":20,"updateTime":20,"relativeEntities":1211,"slug":20,"properties":1212,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1214,"statistic":20},[],{"title":1213},{"EN":41},[],{"id":44,"createTime":20,"updateTime":20,"relativeEntities":1216,"slug":20,"properties":1217,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1219,"statistic":20},[],{"title":1218},{"EN":48},[],[1221,1228],{"id":52,"indexDatabase":1222,"url":63,"indexYears":64,"academicFieldIds":1227,"indexDatabaseRanking":68},{"id":54,"createTime":20,"updateTime":20,"relativeEntities":1223,"label":1224,"description":1225,"key":60,"publicationTags":1226,"standard":20},[],{"EN":57,"VI":57},{"EN":57,"VI":59},[62],[66,67],{"id":70,"indexDatabase":1229,"url":83,"indexYears":20,"academicFieldIds":1234,"indexDatabaseRanking":20},{"id":72,"createTime":20,"updateTime":20,"relativeEntities":1230,"label":1231,"description":1232,"key":79,"publicationTags":1233,"standard":20},[],{"EN":75,"VI":75},{"EN":77,"VI":78},[81,82],[85],{"impactFactor":21,"impactFactorByYear":1236,"i10Index":21,"i10IndexLast5Year":21,"totalPublication":89,"totalPublicationByYear":1237,"totalCitation":21,"totalCitationByYear":1238,"totalCitationPerPublication":21,"totalCitationPerPublicationByYear":1239,"hindexLast5Year":21,"hindex":21},{},{"2001":91,"2003":91,"2004":91,"2005":92,"2006":91,"2007":93,"2008":94,"2009":91,"2010":92,"2011":91,"2012":91,"2015":92,"2017":92,"2018":94,"2019":91,"2020":91,"2022":92,"2023":94},{},{},{"pages":1241,"volume":1243},{"VOID":1242},"833-840",{"VOID":1244},"44",{"total":21,"publishYear":1246,"statisticByYear":1247},2000,{},"2000-12-01","2026-07-18T11:55:05.952+00:00",[68,81],{"id":1252,"createTime":1253,"updateTime":1254,"relativeEntities":1255,"slug":1256,"properties":1257,"entityType":119,"verifyStatus":120,"verifyTime":1268,"verifyNote":122,"languages":20,"translateLanguages":20,"viewCount":21,"primaryUrl":1269,"fullTextUrl":20,"authors":1270,"publicationType":146,"publisherRelationship":1286,"citationCount":20,"citationInfo":20,"publishDate":1338,"publishYear":1339,"citationAnalyzeStatus":1340,"lastCitationAnalyze":1341,"indexDatabases":1342,"openAccess":20,"references":20,"isForceReanalyzing":347},"e02f02a8-ddf2-4e03-8145-eabdee5f6a76","2024-01-03T17:07:32.474+00:00","2026-07-17T10:07:12.525+00:00",[],"Phenomenological-model-for-the-evolution-of-radio-galaxies-such-as-Cygnus-A",{"abstract":1258,"title":1260,"gsPaper":1262,"references":1264,"doi":1266},{"EN":1259},"A phenomenological model for the evolution of classical radio galaxies such as Cygnus A is presented. An activity cycle of the host galaxy in the radio begins with the birth of radio jets, which correspond to shocks on scales ∼1 pc (the radio galaxy B0108+388). In the following stage of the evolution, the radio emission comes predominantly from formations on scales of 10–100 pc, whose physical parameters are close to those of the hot spots of Cygnus A (this corresponds to GHz-peaked spectrum radio sources). Further, the hot spots create radio lobes on scales of 103–104 pc (compact steep-spectrum radio sources). The fully formed radio galaxies have radio jets, hot spots, and giant radio lobes; the direction of the jets can vary in a discrete steps with time, creating new hot spots and inflating the radio lobes (as in Cygnus A). In the final stage of the evolutionary cycle, first the radio jets disappear, then the hot spots, and finally the radio lobes (similar to the giant radio galaxies DA 240 and 3C 236). A large fraction of radio galaxies with repeating activity cycles is observed. The close connection between Cygnus A-type radio galaxies and optical quasars is noted, as well as similarity in the cosmological evolution of powerful radio galaxies and optical quasars.",{"EN":1261},"Phenomenological model for the evolution of radio galaxies such as Cygnus A",{"VOID":1263},"[]",{"VOID":1265},"R. C. Jennison and M. K. Das Gupta, Nature 172, 966 (1954).\nW. Baade and R. Minkowski, Astrophys. J. 119, 206 (1954).\nD. S. de Young and W. I. Axford, Nature 216, 129 (1967).\nM. Ryle and M. S. Longair, Mon. Not.R. Astron.Soc. 136, 123 (1967).\nM. Rees, Nature 229, 312 (1971).\nP. A. G. Scheuer, Mon. Not. R. Astron. Soc. 166, 513 (1974).\nP. J. Hargrave and M. Ryle, Mon.Not. R. Astron. Soc. 166, 305 (1974).\nR. A. Perley, J. W. Dreher, and J. J. Conwan, Astrophys. J. Lett. 285, L35 (1984).\nR. B. Phillips and R. L. Mutel, Astron. Astrophys. 106, 21 (1982).\nJ. C. Carvalho, Mon. Not. R. Astron. Soc. 215, 463 (1985).\nA. C. S. Readhead, G. B. Taylor, T. J. Pearson, and P. N. 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Sci. 759, 87 (1995).",{"VOID":1267},"10.1134\u002FS1063772915060025","2024-06-26T12:51:07.394+00:00","https:\u002F\u002Flink.springer.com\u002Farticle\u002F10.1134\u002FS1063772915060025",[1271],{"id":1272,"sortIndex":21,"researcher":20,"roles":1273,"affiliations":1274,"properties":1283,"displayName":1285,"givenName":20,"familyName":20},"6b69cf54-b06b-49b5-b75f-6610288b125d",[371],[1275],{"id":1276,"sortIndex":21,"affiliation":1277,"properties":20},"2ae41cf8-08e0-44c5-a7c0-5f8e25848e93",{"id":1276,"createTime":20,"updateTime":20,"relativeEntities":1278,"slug":20,"properties":1279,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1282,"statistic":20},[],{"title":1280},{"VI":1281},"Pushchino Radio Astronomy Observatory, Lebedev Physical Institute, Russian Academy of Sciences, Moscow, Russia",[],{"title":1284},{"VI":1285},"V. S. Artyukh",{"url":1269,"publisher":1287,"properties":1333},{"id":6,"createTime":7,"updateTime":8,"relativeEntities":1288,"slug":10,"properties":1289,"entityType":18,"verifyStatus":19,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":21,"subjectFields":1293,"manageAffiliations":1302,"indexDatabases":1313,"url":86,"thumbnailPath":20,"statistic":1328,"gsStatistic":20,"type":97,"analyzePriority":20},[],{"issn":1290,"title":1291,"eissn":1292},{"VOID":13},{"EN":15},{"VOID":17},[1294,1298],{"id":24,"createTime":20,"updateTime":20,"relativeEntities":1295,"label":1296,"description":1297,"parentId":20,"standard":20,"scholarHubFieldId":20},[],{"EN":27},{},{"id":30,"createTime":20,"updateTime":20,"relativeEntities":1299,"label":1300,"description":1301,"parentId":20,"standard":20,"scholarHubFieldId":20},[],{"EN":33},{},[1303,1308],{"id":37,"createTime":20,"updateTime":20,"relativeEntities":1304,"slug":20,"properties":1305,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1307,"statistic":20},[],{"title":1306},{"EN":41},[],{"id":44,"createTime":20,"updateTime":20,"relativeEntities":1309,"slug":20,"properties":1310,"entityType":20,"verifyStatus":20,"verifyTime":20,"verifyNote":20,"languages":20,"translateLanguages":20,"viewCount":20,"url":20,"parentIds":1312,"statistic":20},[],{"title":1311},{"EN":48},[],[1314,1321],{"id":52,"indexDatabase":1315,"url":63,"indexYears":64,"academicFieldIds":1320,"indexDatabaseRanking":68},{"id":54,"createTime":20,"updateTime":20,"relativeEntities":1316,"label":1317,"description":1318,"key":60,"publicationTags":1319,"standard":20},[],{"EN":57,"VI":57},{"EN":57,"VI":59},[62],[66,67],{"id":70,"indexDatabase":1322,"url":83,"indexYears":20,"academicFieldIds":1327,"indexDatabaseRanking":20},{"id":72,"createTime":20,"updateTime":20,"relativeEntities":1323,"label":1324,"description":1325,"key":79,"publicationTags":1326,"standard":20},[],{"EN":75,"VI":75},{"EN":77,"VI":78},[81,82],[85],{"impactFactor":21,"impactFactorByYear":1329,"i10Index":21,"i10IndexLast5Year":21,"totalPublication":89,"totalPublicationByYear":1330,"totalCitation":21,"totalCitationByYear":1331,"totalCitationPerPublication":21,"totalCitationPerPublicationByYear":1332,"hindexLast5Year":21,"hindex":21},{},{"2001":91,"2003":91,"2004":91,"2005":92,"2006":91,"2007":93,"2008":94,"2009":91,"2010":92,"2011":91,"2012":91,"2015":92,"2017":92,"2018":94,"2019":91,"2020":91,"2022":92,"2023":94},{},{},{"pages":1334,"volume":1336},{"VOID":1335},"520-524",{"VOID":1337},"59","2015-06-03",2015,"ERROR_IN_GET_PLATFORM_ID","2026-07-17T10:07:12.524+00:00",[68,81],{"id":1344,"createTime":1345,"updateTime":1346,"relativeEntities":1347,"slug":1348,"properties":1349,"entityType":119,"verifyStatus":120,"verifyTime":1360,"verifyNote":122,"languages":20,"translateLanguages":20,"viewCount":21,"primaryUrl":1361,"fullTextUrl":20,"authors":1362,"publicationType":146,"publisherRelationship":1406,"citationCount":20,"citationInfo":20,"publishDate":1458,"publishYear":1459,"citationAnalyzeStatus":19,"lastCitationAnalyze":1346,"indexDatabases":1460,"openAccess":20,"references":20,"isForceReanalyzing":347},"72fee9a6-0cb1-4def-80f3-6b23a95e4a2d","2023-12-12T16:02:46.547+00:00","2026-07-17T03:58:50.093+00:00",[],"Flares-of-H2O-maser-emission-from-SGR-B2-in-2005-2012",{"abstract":1350,"title":1352,"gsPaper":1354,"references":1356,"doi":1358},{"EN":1351},"We present observations of H2O maser emission from the complex region of active star formation Sgr B2 performed in 2005–2012. The observations were carried out with the 22-m radio telescope of the Pushchino Radio Astronomy Observatory. Seven flares with flux densities higher than 1000 Jy were detected. The flares occurred in all three main sites of star formation in Sgr B2, N,M, and S. The highest peak flux densities were 3200 Jy (60.9 km\u002Fs), 2350 Jy (69.4 km\u002Fs), and 7300 Jy (69.3 km\u002Fs) in N, M, and S, respectively. This last flare was the strongest during our monitoring campaign from 1982 to 2012, both in S and in the entire Sgr B2 complex. Possible associations of the flares were determined. High-velocity, short-lived emission was detected at 124–128 km\u002Fs. Emission at 127 km\u002Fs with a flux density of 23 Jy is associated with region M. Emission at 80.6 and 84.6 km\u002Fs, at radial velocities higher than those observed previously, was detected in region S.",{"EN":1353},"Flares of H2O maser emission from SGR B2 in 2005–2012",{"VOID":1355},"[\"14164519060297030237\"]",{"VOID":1357},"J. M. Bebson and K. J. Johnston, Astrophys. J. 277, 181 (1984).\nS. Y. Liu, D. M. Mehringer, Y. Miao, and E. Snyder, Astrophys. J. 501, 680 (1998).\nH. Kobayashi, M. Ishiguro, Y. Chikada, et al., Publ. Astron. Soc. Jpn. 41, 141 (1989).\nR. A. Gaume, M. J. Claussen, C. G. De Pree, W. M. Gross, and D. M. Mehringer, Astrophys. J. 449, 663 (1995).\nC. G. De Pree, R. A. Gaume, W. M. Goss, and M. J. Claussen, Astrophys. J. 464, 788 (1996).\nP. R. Roelfsema, W. M. Goss, J. B. Whiteoak, et al., Astron. Astrophys. 175, 219 (1987).\nY. J. Kuan and L. E. Snyder, Astrophys. J. 470, 981 (1996).\nD. C. Lis and P. F. Goldsmith, Astrophys. J. 356, 195 (1990).\nS. A. Zhevakin and A. P. Naumov, Izv. Vysh. Uchebn. Zaved., Radiofiz. 6, 674 (1963).\nN. M. Tseitlin, Antenna Engineering and Radioastronomy (Sovetskoe Radio, Moscow, 1976), p. 49 [in Russian].\nO. Ramirez Hernandez, E. E. Lekht, and A. M. Tolmachev, Astron. Rep. 49, 777 (2005).\nE. E. Lekht, O. Ramirez Hernandez, A. M. Tolmachev, et al., Astron. 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Gierlinski, M. Middleton, M. Word, and Ch. Donie, Nature 455, 369 (2008).",{"doi":1594},"10.1038\u002Fnature07277",{"id":20,"text":1596,"url":20,"identifiers":1597},"S. S. Doelman, J. Weintroub, A. E. E. Roders, et al., Nature 455, 78 (2008).",{"doi":1598},"10.1038\u002Fnature07245",{"id":20,"text":1600,"url":20,"identifiers":1601},"A. E. Broderick, A. Loeb, and R. Narayan, Astrophs. J. 701, 1357 (2009).",{"doi":1602},"10.1088\u002F0004-637X\u002F701\u002F2\u002F1357",{"id":20,"text":1604,"url":20,"identifiers":1605},"J. E. Greene, L. C. Ho, and A. J. Barth, Astrophys. J. 688, 159 (2008).",{"doi":1606},"10.1086\u002F592078",{"id":20,"text":1608,"url":20,"identifiers":1609},"J. Kormendy, ASP Conf. Ser. 230, 247 (2001).",{},{"id":20,"text":1611,"url":20,"identifiers":1612},"L. Ferrarese, Astrophys. J. 578, 90 (2002).",{"doi":1613},"10.1086\u002F342308",{"id":20,"text":1615,"url":20,"identifiers":1616},"L. Ferrarese and H. Ford, Space Sci. 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