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DETERMINATION OF PHYSICAL PARAMETERS OF THE W40 HII REGION USING OBSERVATIONS OF Н110𝛼 RADIO RECOMBINATION LINE.
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- Recent Contributions to Physics, 2023, v. 86, n. 3, p. 4, doi. 10.26577/RCPh.2023.v86.i3.01
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A cooperative spectrum sensing method based on information geometry and fuzzy c-means clustering algorithm.
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- EURASIP Journal on Wireless Communications & Networking, 2019, v. 2019, n. 1, p. 1, doi. 10.1186/s13638-019-1338-z
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- Article
A spectroscopic survey of Orion KL between 41.5 and 50 GHz.
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- Astronomy & Astrophysics / Astronomie et Astrophysique, 2017, v. 605, p. 1, doi. 10.1051/0004-6361/201629936
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Supernova Remnants in the Hα and Hβ Lines.
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- Astrophysics, 2017, v. 60, n. 1, p. 1, doi. 10.1007/s10511-017-9458-9
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A multi-line ammonia survey of the Galactic center region with the Tsukuba 32 m telescope. I. Observations and data.
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- Publications of the Astronomical Society of Japan, 2016, v. 68, n. 5, p. 1, doi. 10.1093/pasj/psw072
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A 1.3 cm line survey toward Orion KL.
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- Astronomy & Astrophysics / Astronomie et Astrophysique, 2015, v. 581, p. 1, doi. 10.1051/0004-6361/201526275
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Dense Array Effects in SWIR HgCdTe Photodetecting Arrays.
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- Journal of Electronic Materials, 2015, v. 44, n. 9, p. 3134, doi. 10.1007/s11664-015-3831-4
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Physical parameters of the Orion Bar photodissociation region from radio recombination line observations at 8 mm.
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- Astronomy Letters, 2014, v. 40, n. 10, p. 615, doi. 10.1134/S1063773714100077
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HCO and H observations towards NH sources.
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- Astrophysics & Space Science, 2014, v. 352, n. 2, p. 521, doi. 10.1007/s10509-014-1922-y
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The cometary Hii regions of DR21: Bow shocks or champagne flows or both?⋆,⋆⋆.
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- Astronomy & Astrophysics / Astronomie et Astrophysique, 2014, v. 563, p. 1, doi. 10.1051/0004-6361/201321736
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Determination of the primordial helium abundance from radio recombination line observations: New data. The source W51.
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- Astronomy Letters, 2013, v. 39, n. 11, p. 737, doi. 10.1134/S106377371310006X
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More on the narrowing of impact broadened radio recombination lines at high principal quantum number.
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- Astrophysics & Space Science, 2012, v. 340, n. 1, p. 127, doi. 10.1007/s10509-012-1042-5
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New clues to the impact broadening mystery in radio recombination lines.
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- Astrophysics & Space Science, 2011, v. 335, n. 2, p. 451, doi. 10.1007/s10509-011-0760-4
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Sensitive observations of radio recombination lines in Orion and W51: the data and detection of systematic recombination line blueshifts proportional to impact broadening.
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- Astrophysics & Space Science, 2011, v. 333, n. 2, p. 377, doi. 10.1007/s10509-011-0662-5
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Evolution Strategies in the Multipoint Connections Routing.
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- Radioengineering, 2010, v. 19, n. 3, p. 408
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The Voigt profile of the decameter radio recombination lines and electron density of the expanding CII region towards Cassiopeia A.
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- Astrophysics & Space Science, 2008, v. 318, n. 1/2, p. 35, doi. 10.1007/s10509-008-9881-9
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Investigations of star formation in galaxies using ALMA.
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- Astrophysics & Space Science, 2008, v. 313, n. 1-3, p. 253, doi. 10.1007/s10509-007-9642-1
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GMRT and VLA Observations at 49 cm and 20 cm of the HII Region near l = 24.8°, b = 0.1°.
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- Journal of Astrophysics & Astronomy, 2007, v. 28, n. 1, p. 51, doi. 10.1007/s12036-007-0005-7
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Effective temperature of the star ϑ1 Ori C.
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- Astronomy Letters, 2007, v. 33, n. 1, p. 34, doi. 10.1134/S1063773707010045
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The Radio Recombination Line Intensities Of Atoms And Ions: Helium, Carbon And Oxygen.
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- Astrophysics & Space Science, 2005, v. 300, n. 4, p. 357, doi. 10.1007/s10509-005-4499-7
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Transmission-line matrix models for solving transient problems of diffusion with recombination.
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- International Journal of Numerical Modelling, 2003, v. 16, n. 5, p. 453, doi. 10.1002/jnm.511
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Physical Conditions in Photodissociation Regions from Observations of Carbon Radio Recombination Lines and IR Fine-Structure Lines of CII and OI.
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- Astronomy Reports, 2000, v. 44, n. 7, p. 426, doi. 10.1134/1.163867
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High resolution radio recombination line observations.
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- Astronomy & Astrophysics Review, 1992, v. 4, n. 2, p. 161, doi. 10.1007/BF00874056
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