Search

Your search keyword '"Belyaev, D.A."' showing total 11 results
Start Over Author "Belyaev, D.A."
11 results on '"Belyaev, D.A."'

2. Structure of a shell made from uranium alloyed with iron and germanium after explosive loading

Author

Belyaev D.A., Aleksandrov A.S., Zuev Yu.N., Kozlov E.A., Shestakov A.E., Lekomtsev S.A., Nedosviti A.S., Svyatov I.L., and Levi E.A.

Subjects
Physics, QC1-999
Abstract

This paper presents results of metallographic examination of a thick-wall spherical shell from uranium alloyed with iron and germanium. This shell is recovered after low-level explosive loading. Light microscopy, hardness measurement, scanning electron microscopy and X-Ray diffraction study were used to investigate the meridional section of the test shell as this section most completely exhibits the whole variety of structural features associated with explosive loading of the material. Processing, presentation, and analysis of experimental data on volumetric distribution of studied physical quantities were performed with the help of digital panning and color mapping.

Published
2021
Full Text
View/download PDF

6. Solar infrared occultation observations by SPICAM experiment on Mars-Express: Simultaneous measurements of the vertical distributions of H.sub.2O, CO.sub.2 and aerosol

Author

Fedorova, A.A., Korablev, O.I., Bertaux, J.-L., Rodin, A.V., Montmessin, F., Belyaev, D.A., and Reberac, A.

Subjects
Atmospheric physics -- Measurement, Atmospheric physics -- Optical properties, Atmospheric physics -- Analysis, Mars (Planet) -- Measurement, Mars (Planet) -- Optical properties, Mars (Planet) -- Analysis, Clouds -- Measurement, Clouds -- Optical properties, Clouds -- Analysis, Water -- Measurement, Water -- Optical properties, Water -- Analysis, Atmospheric density -- Measurement, Atmospheric density -- Optical properties, Atmospheric density -- Analysis, Altitudes -- Measurement, Altitudes -- Optical properties, Altitudes -- Analysis, Planets -- Atmosphere, Planets -- Measurement, Planets -- Optical properties, Planets -- Analysis, Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2008.11.006 Byline: A.A. Fedorova (a), O.I. Korablev (a), J.-L. Bertaux (b)(c), A.V. Rodin (a)(d), F. Montmessin (b)(c), D.A. Belyaev (a), A. Reberac (b)(c) Keywords: Mars; atmosphere; Spectroscopy Abstract: The infrared AOTF spectrometer is a part of the SPICAM experiment onboard the Mars-Express ESA mission. The instrument has a capability of solar occultations and operates in the spectral range of 1-1.7 [mu]m with a spectral resolution of [approximately equal to]3.5 cm.sup.-1. We report results from 24 orbits obtained during MY28 at L.sub.s 130[degrees]-160[degrees], and the latitude range of 40[degrees]-55[degrees] N. For these orbits the atmospheric density from 1.43 [mu]m CO.sub.2 band, water vapor mixing ratio based on 1.38 [mu]m absorption, and aerosol opacities were retrieved simultaneously. The vertical resolution of measurements is better than 3.5 km. Aerosol vertical extinction profiles were obtained at 10 wavelengths in the altitude range from 10 to 60 km. The interpretation using Mie scattering theory with adopted refraction indices of dust and H.sub.2O ice allows to retrieve particle size (r.sub.eff[approximately equal to]0.5-1 [mu]m) and number density ([approximately equal to]1 cm.sup.-3 at 15-30 km) profiles. The haze top is generally below 40 km, except the longitude range of 320[degrees]-50[degrees] E, where high-altitude clouds at 50-60 km were detected. Optical properties of these clouds are compatible with ice particles (effective radius r.sub.eff=0.1-0.3[mu]m, number density N[approximately equal to]10 cm.sup.-3) distributed with variance [nu].sub.eff=0.1-0.2[mu]m. The vertical optical depth of the clouds is below 0.001 at 1 [mu]m. The atmospheric density profiles are retrieved from CO.sub.2 band in the altitude range of 10-90 km, and H.sub.2O mixing ratio is determined at 15-50 km. Unless a supersaturation of the water vapor occurs in the martian atmosphere, the H.sub.2O mixing ratio indicates [approximately equal to]5 K warmer atmosphere at 25-45 km than predicted by models. Author Affiliation: (a) Space Research Institute (IKI), 84/32 Profsoyuznaya, 117997 Moscow, Russia (b) Service d'Aeronomie du CNRS, BP 3, 91371, Verrieres-le-Buisson, France (c) Institut Pierre Simon Laplace, Universite de Versailles-Saint-Quentin, 78 Saint Quentin en Yvelines, France (d) Moscow Institute of Physics and Technology, Institutsky dr. 9, 141700 Dolgoprudnyi, Russia Article History: Received 26 November 2007; Revised 28 July 2008; Accepted 3 November 2008

Published
2009

8. Experimental Studies of the Potential Use of Virtual Reality Systems When Modeling the Lunokhod Controlled Movement on the Centrifuge.

Author

Dolgov, P.P., primary, Kirshanov, V.N., additional, Irodov, E.Yu., additional, Gavrik, I.N., additional, Korennoy, V.S., additional, Onufrienko, Yu.I., additional, Chudinov, A.P., additional, Ivashchuk, O.B., additional, Belyaev, A.N., additional, Grishina, I.A., additional, Belyavtsev, S.N., additional, Belyaev, D.A., additional, Bulgakov, A.V., additional, Shvetsov, V.V., additional, Kaspransky, R.R., additional, Zaveryukha, A.S., additional, Konovalova, I.V., additional, Sukhochev, P.Yu., additional, Latonov, V.V., additional, Bugriy, G.S., additional, and Chertopolokhov, V.A., additional

Published
2020
Full Text
View/download PDF

9. No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations

Author

Belgian Science Policy Office, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Centre National de la Recherche Scientifique (France), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Russian Government, Agenzia Spaziale Italiana, European Space Agency, Korablev, O., Vandaele, Ann Carine, Montmessin, Franck, Fedorova, A. A., Trokhimovskiy, A., Forget, François, Lefèvre, F., Daerden, Frank, Thomas, Ian R., Trompet, L., Erwin, Justin T., Aoki, Shohei, Robert, S., Neary, L., Viscardy, S., Grigoriev, A.V., Ignatiev, N. I., Shakun, Alexey, Patrakeev, A., Belyaev, D.A., Bertaux, J.L., Olsen, K. S., Baggio, L., Alday, J., Ivanov, Y. S., Ristic, Bojan, Mason, J., Willame, Y., Depiesse, C., Hetey, L., Berkenbosch, S., Clairquin, R., Queirolo, C., Beeckman, B., Neefs, E., Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Wilson, C. F., Etiope, G., Zelenyi, Lev, Svedhem, H., Vago, J. L., Alonso-Rodrigo, G., Altieri, F., Anufreychik, K., Arnold, G., Bauduin, S., Bolsée, D., Funke, Bernd, García Comas, Maia, González-Galindo, F., López-Puertas, Manuel, López-Valverde, M. A., Martín-Torres, F. J., Vazquez, L., Zorzano, María Paz, Belgian Science Policy Office, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Centre National de la Recherche Scientifique (France), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Russian Government, Agenzia Spaziale Italiana, European Space Agency, Korablev, O., Vandaele, Ann Carine, Montmessin, Franck, Fedorova, A. A., Trokhimovskiy, A., Forget, François, Lefèvre, F., Daerden, Frank, Thomas, Ian R., Trompet, L., Erwin, Justin T., Aoki, Shohei, Robert, S., Neary, L., Viscardy, S., Grigoriev, A.V., Ignatiev, N. I., Shakun, Alexey, Patrakeev, A., Belyaev, D.A., Bertaux, J.L., Olsen, K. S., Baggio, L., Alday, J., Ivanov, Y. S., Ristic, Bojan, Mason, J., Willame, Y., Depiesse, C., Hetey, L., Berkenbosch, S., Clairquin, R., Queirolo, C., Beeckman, B., Neefs, E., Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Wilson, C. F., Etiope, G., Zelenyi, Lev, Svedhem, H., Vago, J. L., Alonso-Rodrigo, G., Altieri, F., Anufreychik, K., Arnold, G., Bauduin, S., Bolsée, D., Funke, Bernd, García Comas, Maia, González-Galindo, F., López-Puertas, Manuel, López-Valverde, M. A., Martín-Torres, F. J., Vazquez, L., and Zorzano, María Paz

Abstract

The detection of methane on Mars has been interpreted as indicating that geochemical or biotic activities could persist on Mars today1. A number of different measurements of methane show evidence of transient, locally elevated methane concentrations and seasonal variations in background methane concentrations2–5. These measurements, however, are difficult to reconcile with our current understanding of the chemistry and physics of the Martian atmosphere6,7, which—given methane’s lifetime of several centuries—predicts an even, well mixed distribution of methane1,6,8. Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. We did not detect any methane over a range of latitudes in both hemispheres, obtaining an upper limit for methane of about 0.05 parts per billion by volume, which is 10 to 100 times lower than previously reported positive detections2,4. We suggest that reconciliation between the present findings and the background methane concentrations found in the Gale crater4 would require an unknown process that can rapidly remove or sequester methane from the lower atmosphere before it spreads globally. © 2019, The Author(s), under exclusive licence to Springer Nature Limited.

Published
2019

10. Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author

Ministerio de Ciencia e Innovación (España), European Space Agency, Belgian Science Policy Office, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Centre National de la Recherche Scientifique (France), Russian Government, Vandaele, Ann Carine, Korablev, O., Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, F., López-Valverde, M. A., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Erwin, Justin T., Trompet, L., Fedorova, A. A., Montmessin, Franck, Trokhimovskiy, A., Belyaev, D.A., Ignatiev, N. I., Luginin, M., Olsen, K. S., Baggio, L., Alday, J., Bertaux, J.L., Betsis, D., Bolsée, D., Clancy, R. Todd, Cloutis, E., Depiesse, C., Funke, Bernd, García Comas, Maia, Gérard, Jean-Claude, Giuranna, M., González-Galindo, F., Grigoriev, A.V., Ivanov, Y. S., Kaminski, J., Karatekin, O., Lefèvre, F., Lewis, S., López-Puertas, Manuel, Mahieux, A., Maslov, I., Mason, J., Mumma, M.J., Neary, L., Neefs, E., Patrakeev, A., Patsaev, D., Ristic, Bojan, Robert, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Martín-Torres, F. J., Vazquez, L., Zorzano, María Paz, Ministerio de Ciencia e Innovación (España), European Space Agency, Belgian Science Policy Office, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Centre National de la Recherche Scientifique (France), Russian Government, Vandaele, Ann Carine, Korablev, O., Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, F., López-Valverde, M. A., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Erwin, Justin T., Trompet, L., Fedorova, A. A., Montmessin, Franck, Trokhimovskiy, A., Belyaev, D.A., Ignatiev, N. I., Luginin, M., Olsen, K. S., Baggio, L., Alday, J., Bertaux, J.L., Betsis, D., Bolsée, D., Clancy, R. Todd, Cloutis, E., Depiesse, C., Funke, Bernd, García Comas, Maia, Gérard, Jean-Claude, Giuranna, M., González-Galindo, F., Grigoriev, A.V., Ivanov, Y. S., Kaminski, J., Karatekin, O., Lefèvre, F., Lewis, S., López-Puertas, Manuel, Mahieux, A., Maslov, I., Mason, J., Mumma, M.J., Neary, L., Neefs, E., Patrakeev, A., Patsaev, D., Ristic, Bojan, Robert, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Martín-Torres, F. J., Vazquez, L., and Zorzano, María Paz

Abstract

Global dust storms on Mars are rare1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere. © 2019, The Author(s), under exclusive licence to Springer Nature Limited.

Published
2019

11. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, Franck, Trokhimovskiy, A., Fedorova, A.A., Shakun, A.V., Grigoriev, A.V., Moshkin, B.E., Ignatiev, N.I., Forget, F., Lefevre, F., Anufreychik, A., Dzuban, I., Ivanov, Y.S., Kalinnikov, Y.K., Kozlova, T. O., Kungurov, A., Markov, V., Martynovich, F., Mazlov, I., Merzlyakov, D., Moiseev, P.P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripo, A., Sazonov, O., Semena, N., Shashkin, V., Sidorov, A., Stepanov, A.V., Stupin, I., Timonin, D., Titov, A.Y., Viktorov, A., Zharkov, A., Alteri, F., Arnold, G., Belyaev, D.A., Bertaux, J.-L., Betsis, D.S., Duxbury, N., Encrenaz, T., Fouchet, T., Gerard, J.-C., Grassi, D., Guerlet, S., Hargtogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V.A., Kuzmin, R.O., Lellouch, E., Lopez-Valverde, M.A., Luginin, M., Määttänen, A., Marcq, M., Martin Torres, J., Medvedev, A.S., Millour, E., Olsen, K.S., Patel, M.R., Quantin-Nataf, C., Rodin, A.V., Shematovich, V.I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C.F., Zazova, L.V., Zelenyi, L.M., Zorzano, M.P., Russian Science Foundation, Ministerio de Economía y Competitividad (España), Svedhem, H., and Russel, C.T.

Subjects
Leitungsbereich PF, Mars · Atmosphere · High-resolution spectrometer · Fourier-spectrometer ·Echelle · Cross-dispersion
Abstract

The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described., ExoMars is a space mission by ESA and Roscosmos. The development and fabrication of ACS was funded by Roscosmos with contributions from LATMOS (France) funded by CNES. Science operations are funded by Roscosmos and ESA. AAF, NII, DAB, JLB, DSB, ML acknowledge the grant #14.W03.31.0017 of Ministry for Education and Science of Russian Federation for science support of the ACS experiment. AT, AVS, and BEM acknowledge support from Russian Science Foundation (grant RSF 16-12-10453), whichenabledassessmentofmeasurementcharacteristicsoftheinstrument andtheassociated modeling. LMZ acknowledges RSF funding (grant RSF 16-42-01103). Other authors affiliated with IKI acknowledge FANO, contracts 0120.06 02993 (0028-2014-0004) and 0120.03 03422 (0028-2014-0007). MRP acknowledges funding under the UK Space Agency grant ST/I003061/1 and ST/P001262/1. LV acknowledges the support of Ministerio de Economía y Competitividad of Spain under project ESP2016-79135-R. We are grateful to Richard Zurek and an anonymous reviewer for useful comments and suggestions, which helped improving this paper. We thank Sylvain Cnudde, Evgeny Germanyuk, and Ekaterina Korableva for help in rendering graphics. We also express our sincere gratitude to the space agencies, countries, companies, and project teams who made the ExoMars 2016 mission possible.

Published
2017

Catalog

Books, media, physical & digital resources
See catalog results