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9. The Project 'Analogs for VENus’s GEologically Recent Surfaces' (AVENGERS): A Comprehensive Database of Terrestrial Active Volcanoes for the Analysis of Ongoing Volcanism on Venus

Author

D'Incecco, Piero, Filiberto, Justin, Garvin, B., Arney, G. N., Getty, S. A., Di Achille, Gaetano, Ghail, R., Zelenyi, L. M., Zasova, L. V., Ivanov, M. A., Gorinov, D. A., Bruzzone, L., Bhattacharya, S., Bhiravarasu, S. S., Putrevu, D., Monaco, Carmelo, Branca, Stefano., Aveni, Simone Salvatore, López, Iván, Eggers, Gabriel L., Mari, Nicola, Blackett, Matthew, Mastrogiuseppe, Marco, Komatsu, Goro, Kosenkova, A., Ahrens, C., Cardinale, M., and El Yazidi, Mayssa

Published
2023

11. Venera-D Mission Concept to Study Atmosphere, Surface and Plasma Environment: Phase II Report of the Venera-D Joint Science Definition Team

Author

Zasova, L, Gregg, T, Burdanov, A, Economou, T, Eismont, N, Gerasimov, M, Gorinov, D, Hall, J, Ignatiev, N, Ivanov, M, Jessup, K. L, Khatuntsev, I, Korablev, O, Kremic, T, Limaye, S, Lomakin, I, Martynov, A, Ocampo, A, Vaisberg, O, Voron, V, and Vorontsov, V

Subjects
Lunar And Planetary Science And Exploration
Abstract

Venus and Earth were formed approximately the same distance from the Sun, and have almost the same masses and volumes: they should be the most similar pair of planets in the Solar System. A vital, outstanding question is how and when these planets diverged in their atmospheric evolutions. Significantly, recent investigations present evidence for microbial life in Venus' cloud deck. Venus presents us with fundamental questions about the origin and evolution of planetary bodies and life in our Solar System.Venera-D (D stands for the Russian word for "long-lived:" dolgozhivushaya) is a potential mission that would combine simultaneous observations of Venus' atmosphere, plasma environment, and surface to try to answer these essential questions.

Published
2018

12. Martian Atmospheric Thermal Structure and Dust Distribution During the MY 34 Global Dust Storm From ACS TIRVIM Nadir Observations

Author

Vlasov, P., primary, Ignatiev, N., additional, Guerlet, S., additional, Grassi, D., additional, Korablev, O., additional, Grigoriev, А., additional, Shakun, A., additional, Patsaev, D., additional, Maslov, I., additional, Zasova, L., additional, Luginin, M., additional, Trokhimovskiy, A., additional, Millour, E., additional, Forget, F., additional, Haus, R., additional, Arnold, G., additional, and Montmessin, F., additional

Published
2022
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13. O2 (а1Δg) Airglow at 1.27 μM and upper Mesosphere Dynamics on the Night Side of Venus.

Author

Shakun, A. V., Zasova, L. V., Gorinov, D. A., Khatuntsev, I. V., Ignatiev, N. I., Patsaeva, M. V., and Turin, A. V.

Subjects
*MESOSPHERE, *AIRGLOW, *VENUSIAN atmosphere, *VENUS (Planet), *ATMOSPHERIC boundary layer
Abstract

This research studies the O2 (a1Δg) nightglow distribution in 1.27 μm to understand the dynamics of the atmosphere of Venus. Several factors were considered in the retrieval process, such as thermal emission of the lower atmosphere, reflection by the clouds. Results show deviation from SS-AS circulation mode: the area where horizontal flows from the dayside converge and where oxygen recombines and emits shifts from the midnight to 22–23 hours local time. This shift is caused by solar-induced thermal tide on Venus nightside. Some conclusions about the upper mesosphere dynamics are also presented. [ABSTRACT FROM AUTHOR]

Published
2023
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14. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., 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., Zasova, L. V., Zelenyi, L. M., and Zorzano, M. P.

Published
2017
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15. Status report of the Venera-D Joint Science Definition Team

Author

Vorontsov, V, Vaisberg, O, Teselkin, S, Ocampo, A, Martynov, A, Lomakin, I, Limaye, S, Kremic, T, Korablev, O, Khatuntsev, I, Lea Jessup, K, Ivanov, M, Ignatiev, N, Hall, J, Gorinov, D, Gerasimov, M, Eismont, N, Economou, T, Burdanov, A, Zasova, L, and Senske, D

Abstract

UNKNOWN

Published
2017

16. Status report of the Venera-D Joint Science Definition Team

Author

Senske, D, Zasova, L, Burdanov, A, Economou, T, Eismont, N, Gerasimov, M, Gorinov, D, Hall, J, Ignatiev, N, Ivanov, M, Lea Jessup, K, Khatuntsev, I, Korablev, O, Kremic, T, Limaye, S, Lomakin, I, Martynov, A, Ocampo, A, Teselkin, S, Vaisberg, O, and Vorontsov, V

Published
2017

20. AOST: Fourier spectrometer for studying mars and phobos

Author

Korablev, O. I., Grigor’ev, A. V., Moshkin, B. E., Zasova, L. V., Montmessin, F., Gvozdev, A. B., Shashkin, V. N., Patsaev, D. V., Makarov, V. S., Maksimenko, S. V., Ignatiev, N. I., Fedorova, A. A., Arnold, G., Shakun, A. V., Terentiev, A. I., Zharkov, A. V., Mayorov, B. S., Nikol’sky, Yu. V., Khatuntsev, I. V., Bellucci, G., Giuranna, M., Kuz’min, R. O., and Rodin, A. V.

Published
2012
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23. New in the physics of planetary atmosphere

Author

Korablev, O. I., Zasova, L. V., Fedorova, A. A., Rodin, A. V., Ignatiev, N. I., Breus, T. K., Izakov, M. N., Maiorov, B. S., Krivolutsky, A. A., Petrova, E. V., Ivanov, A. Yu., and Trokhimovskii, A. Yu.

Published
2009
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24. European Venus Explorer (EVE): an in-situ mission to Venus

Author

Chassefière, E., Korablev, O., Imamura, T., Baines, K. H., Wilson, C. F., Titov, D. V., Aplin, K. L., Balint, T., Blamont, J. E., Cochrane, C. G., Ferencz, Cs., Ferri, F., Gerasimov, M., Leitner, J. J., Lopez-Moreno, J., Marty, B., Martynov, M., Pogrebenko, S. V., Rodin, A., Whiteway, J. A., Zasova, L. V., Michaud, J., Bertrand, R., Charbonnier, J.-M., Carbonne, D., Raizonville, P., and EVE team

Published
2009
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25. O.sub.2 1.27[mu]m emission maps as derived from OMEGA/MEx data

Author

Altieri, F., Zasova, L., D'Aversa, E., Bellucci, G., Carrozzo, F.G., Gondet, B., and Bibring, J.-P.

Subjects
Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2009.07.022 Byline: F. Altieri (a), L. Zasova (b), E. D'Aversa (a), G. Bellucci (a), F.G. Carrozzo (a), B. Gondet (c), J.-P. Bibring (c) Keywords: Mars; Atmosphere; Atmosphere; Composition; Spectroscopy Abstract: We present a method to derive the 2D maps of the O.sub.2 (a.sup.1 [DELTA].sub.g) airglow emission at 1.27[mu]m from the OMEGA/MEx nadir observations. The OMEGA imaging capabilities allow monitoring the 2D distribution, daily and seasonal variation of the O.sub.2 emission intensities with a detection limit of 4 MR. The highest values, of the order of [approximately equal to]31 MR, are found on the south pole for 11h Atmospheric waves crossing the terminator on the southern polar regions are observed for the first time during the MY28 early spring. The spatial scale of the waves ranges from 100 to 130km, and the intensity fluctuations are of the order of 4MR. This study confirms the high potentiality of O.sub.2 (a.sup.1 [DELTA].sub.g) day glow as a passive tracer of the martian atmosphere dynamics at high latitudes. Author Affiliation: (a) IFSI - INAF, Via del Fosso del Cavaliere 100, 00133 Rome, Italy (b) Space Research Institute, 84/32 Profsoyuznaya Str., 117997 Moscow, Russia (c) Institut d'Astrophysique Spatiale, BAcentst. 121, Universite Paris-Sud, 91405 Orsay Cedex, France Article History: Received 22 July 2008; Revised 18 June 2009; Accepted 6 July 2009

Published
2009

26. PFS/MEX observations of the condensing CO.sub.2 south polar cap of Mars

Author

Giuranna, M., Grassi, D., Formisano, V., Montabone, L., Forget, F., and Zasova, L.

Subjects
Mars (Planet) -- 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.2008.05.019 Byline: M. Giuranna (a)(b), D. Grassi (a), V. Formisano (a), L. Montabone (c)(d), F. Forget (d), L. Zasova (a)(e) Keywords: Mars; polar caps; Mars; climate; Ices Abstract: The condensing CO.sub.2 south polar cap of Mars and the mechanisms of the CO.sub.2 ice accumulation have been studied through the analysis of spectra acquired by the Planetary Fourier Spectrometer (PFS) during the first two years of ESA's Mars Express (MEX) mission. This dataset spans more than half a martian year, from Ls[approximately equal to]330[degrees] to Ls[approximately equal to]194[degrees], and includes the southern fall season which is found to be extremely important for the study of the residual south polar cap asymmetry. The cap expands symmetrically and with constant speed during the fall season. The maximum extension occurs sometime in the 80[degrees]-90[degrees]Ls range, when the cap edges are as low as -40[degrees] latitude. Inside Hellas and Argyre basins, frost can be stable at lower latitudes due to the higher pressure values, causing the seasonal cap to be asymmetric. Within the seasonal range considered in this paper, the cap edge recession rate is approximately half the rate at which the cap edge expanded. The longitudinal asymmetries reduce during the cap retreat, and disappear around Ls[approximately equal to]145[degrees]. Two different mechanisms are responsible for CO.sub.2 ice accumulation during the fall season, especially in the 50[degrees]-70[degrees]Ls range. Here, CO.sub.2 condensation in the atmosphere, and thus precipitation, is allowed exclusively in the western hemisphere, and particularly in the longitudinal corridor of the perennial cap. In the eastern hemisphere, the cap consists mainly of CO.sub.2 frost deposits, as a consequence of direct vapor deposition. The differences in the nature of the surface ice deposits are the main cause for the residual south polar cap asymmetry. Results from selected PFS orbits have also been compared with the results provided by the martian general circulation model (GCM) of the Laboratoire de Meteorologie dynamique (LMD) in Paris, with the aim of putting the observations in the context of the global circulation. This first attempt of cross-validation between PFS measurements and the LMD GCM on the one hand confirms the interpretation of the observations, and on the other hand shows that the climate modeling during the southern polar night on Mars is extremely sensitive to the dynamical forcing. Author Affiliation: (a) Istituto di Fisica dello Spazio Interplanetario INAF-IFSI, Via del Fosso del Cavaliere 100, 00133 Roma, Italy (b) Centro Interdipartimentale di Studi e Attivita Spaziali CISAS - 'G. Colombo,' University of Padova, Via Venezia 15, 35131 Padova, Italy (c) Department of Physics & Astronomy, The Open University, Walton Hall, Milton Keynes MK7 6AA, United Kingdom (d) Laboratoire de Meteorologie Dynamique du CNRS, Universite Paris 6, BP99, 75252, Paris Cedex 05, France (e) Space Research Institute of Russian Academy of Sciences (IKI), Profsojuznaja 84/32, 117810 Moscow, Russia Article History: Received 20 November 2007; Revised 4 April 2008

Published
2008

27. South-polar features on Venus similar to those near the north pole

Author

Piccioni, G., Drossart, P., Sanchez-Lavega, A., Hueso, R., Taylor, F. W., Wilson, C. F., Grassi, D., Zasova, L., Moriconi, M., Adriani, A., Lebonnois, S., Coradini, A., Bézard, B., Angrilli, F., Arnold, G., Baines, K. H., Bellucci, G., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M. I., Carlson, R. W., Di Lellis, A., Encrenaz, T., Erard, S., Fonti, S., Formisano, V., Fouchet, T., Garcia, R., Haus, R., Helbert, J., Ignatiev, N. I., Irwin, P. G. J., Langevin, Y., Lopez-Valverde, M. A., Luz, D., Marinangeli, L., Orofino, V., Rodin, A. V., Roos-Serote, M. C., Saggin, B., Stam, D. M., Titov, D., Visconti, G., and Zambelli, M.

Published
2007
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28. A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express

Author

Drossart, P., Piccioni, G., Gérard, J. C., Lopez-Valverde, M. A., Sanchez-Lavega, A., Zasova, L., Hueso, R., Taylor, F. W., Bézard, B., Adriani, A., Angrilli, F., Arnold, G., Baines, K. H., Bellucci, G., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M. I., Carlson, R. W., Coradini, A., Di Lellis, A., Encrenaz, T., Erard, S., Fonti, S., Formisano, V., Fouchet, T., Garcia, R., Haus, R., Helbert, J., Ignatiev, N. I., Irwin, P., Langevin, Y., Lebonnois, S., Luz, D., Marinangeli, L., Orofino, V., Rodin, A. V., Roos-Serote, M. C., Saggin, B., Stam, D. M., Titov, D., Visconti, G., Zambelli, M., and Tsang, C.

Published
2007
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29. Why We Need a Long-Term Sustainable Venus Program

Author

Helbert, Jörn, Dyar, Melinda, Izenberg, N. R., Ghail, Richard, Garvin, J., Byrne, Paul, Smrekar, Suzanne E., Gilmore, M., Widemann, Thomas, Beauchamp, Patricia M., Shaji, Nigar, and Zasova, L.

Subjects
Radar, Lander, Missionen, Planetare Labore, Spektroskopie, Venus
Published
2020

31. Results of measurements with the Planetary Fourier Spectrometer onboard Mars Express: Clouds and dust at the end of southern summer. A comparison with OMEGA images

Author

Zasova, L. V., Formisano, V., Moroz, V. I., Bibring, J. -P., Grassi, D., Ignatiev, N. I., Giuranna, M., Bellucci, G., Altieri, F., Blecka, M., Gnedykh, V. N., Grigoriev, A. V., Lellouch, E., Mattana, A., Maturilli, A., Moshkin, B. E., Nikolsky, Yu. V., Patsaev, D. V., Piccioni, G., Ratai, M., Saggin, B., Fonti, S., Khatuntsev, I. V., Hirsh, H., and Ekonomov, A. P.

Published
2006
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33. A warm layer in Venus' cryosphere and high-altitude measurements of HF, HCl, H2O and HDO

Author

Bertaux, Jean-Loup, Vandaele, Ann-Carine, Korablev, Oleg, Villard, E., Fedorova, A., Fussen, D., Quemerais, E., Belyaev, D., Mahieux, A., Montmessin, F., Muller, C., Neefs, E., Nevejans, D., Wilquet, V., Dubois, J. P., Hauchecorne, A., Stepanov, A., Vinogradov, I., Rodin, A., Cabane, M., Chassefiere, E., Chaufray, J. Y., Dimarellis, E., Leblanc, F., Lefevre, F., Rannou, P., Van Ransbeeck, E., Zasova, L., Forget, F., Lebonnois, S., Titov, D., Rafkin, S., Durry, G., Gerard, J. C., and Sandel, B.

Subjects
Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): Jean-Loup Bertaux [1, 2, 5]; Ann-Carine Vandaele [3]; Oleg Korablev [4]; E. Villard [1, 2, 5]; A. Fedorova [4]; D. Fussen [3]; E. Quémerais [1, 2, 5]; D. Belyaev [...]

Published
2007
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36. Phyllosilicates on Mars and implications for early martian climate

Author

Poulet, F., Bibring, J.-P., Mustard, J. F., Gendrin, A., Mangold, N., Langevin, Y., Arvidson, R. E., Gondet, B., Gomez, C., Berthe, M., Erard, S., Forni, O., Manaud, N., Poulleau, G., Soufflot, A., Combes, M., Drossart, P., Encrenaz, T., Fouchet, T., Melchiorri, R., Bellucci, G., Altieri, F., Formisano, V., Fonti, S., Capaccioni, F., Cerroni, P., Coradini, A., Korablev, O., Kottsov, V., Ignatiev, N., Titov, D., Zasova, L., Pinet, P., Schmitt, B., Sotin, C., Hauber, E., Hoffmann, H., Jaumann, R., Keller, U., Arvidson, R., Mustard, J., and Forget, F.

Subjects
Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): F. Poulet (corresponding author) [1]; J.-P. Bibring [1]; J. F. Mustard [2]; A. Gendrin [2]; N. Mangold [3]; Y. Langevin [1]; R. E. Arvidson [4]; B. Gondet [1]; C. [...]

Published
2005
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37. Winds From the Visible (513 nm) Images Obtained by the Venus Monitoring Camera Onboard Venus Express.

Author

Khatuntsev, I. V., Patsaeva, M. V., Zasova, L. V., Titov, D. V., Ignatiev, N. I., Gorinov, D. A., and Turin, A. V.

Subjects
VENUS (Planet), VENUSIAN atmosphere, ZONAL winds, MERIDIONAL winds, WIND speed
Abstract

We present more than 250,000 wind vectors derived from the visible (513 nm) images captured by the Venus Monitoring Camera (VMC) onboard ESA's Venus Express orbiter in the Southern hemisphere from 01 July 2007 to 29 January 2013. From comparison to the wind velocity derived from tracking of the descent probes, these measurements correspond to 60 ± 3 km altitude, being between two levels 70 ± 2 km and 55 ± 2 km, probed by VMC in ultraviolet (UV) (365 nm) and NIR (965 nm) channels, respectively. The mean zonal wind suggests retrograde circulation with mean zonal wind speed decreasing from 76.5 to 61.5 m/s at 30°–65°S. In low latitudes, 10–20°S, it increased to 82 m/s over the course of the mission. The mean zonal flow depends on local solar time and latitude and is affected by the large‐scale topography. The meridional winds indicated equatorward flow of up to 7 m/s in the middle and low cloud opposite to that derived from simultaneous UV observations at the cloud top. Plain Language Summary: Dynamics of the Venus atmosphere is dominated by a strong zonal retrograde circulation called "superrotation." The physical mechanisms maintaining this unique regime are poorly understood due to insufficient observational data. For about eight years, the Venus Monitoring Camera onboard ESA's Venus Express orbiter monitored motions of the cloud features in three spectral ranges: ultraviolet (UV) (365 nm), visible (513 nm), and near‐infrared (915 nm). These wavelengths probed different altitudes: 70 ± 2 km, 60 ± 3 km, and 55 ± 2 km correspondingly, thus providing wind field tomography. In this paper, we present more than 250,000 wind vectors derived from the visible images. The results suggest decrease of the retrograde mean zonal wind speed from 76.5 to 61.5 m/s at 30°–65°S, and its increase up to 82 m/s at 10–20°S and show pronounced variations with local solar time, latitude, and surface topography. Interestingly, the meridional winds indicate equatorward flow of up to 7 m/s in the deep cloud opposite to that previously derived from UV images at the cloud top. Key Points: More than 250,000 wind vectors at 57–63 km altitude were derived from the images taken by the Venus Monitoring Camera /Venus Express visible (513 nm) channelMean zonal wind speed accelerated by ∼18.5 m/s at 30 ± 5°S over 8 Venusian yearsZonal wind speed decreased from 85 m/s at the equator to 35 m/s at 80°S, meridional wind of up to 7 m/s velocity is directed equatorward [ABSTRACT FROM AUTHOR]

Published
2022
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38. The planetary fourier spectrometer (PFS) onboard the European Venus Express mission

Author

Formisano, V., Angrilli, F., Arnold, G., Atreya, S., Baines, K.H., Bellucci, G., Bezard, B., Billebaud, F., Biondi, D., Blecka, M.I., Colangeli, L., Comolli, L., Crisp, D., D’Amore, M., Encrenaz, T., Ekonomov, A., Esposito, F., Fiorenza, C., Fonti, S., Giuranna, M., Grassi, D., Grieger, B., Grigoriev, A., Helbert, J., Hirsch, H., Ignatiev, N., Jurewicz, A., Khatuntsev, I., Lebonnois, S., Lellouch, E., Mattana, A., Maturilli, A., Mencarelli, E., Michalska, M., Lopez Moreno, J., Moshkin, B., Nespoli, F., Nikolsky, Yu., Nuccilli, F., Orleanski, P., Palomba, E., Piccioni, G., Rataj, M., Rinaldi, G., Rossi, M., Saggin, B., Stam, D., Titov, D., Visconti, G., and Zasova, L.

Published
2006
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39. The Planetary Fourier Spectrometer (PFS) onboard the European Mars Express mission

Author

Formisano, V., Angrilli, F., Arnold, G., Atreya, S., Bianchini, G., Biondi, D., Blanco, A., Blecka, M.I., Coradini, A., Colangeli, L., Ekonomov, A., Esposito, F., Fonti, S., Giuranna, M., Grassi, D., Gnedykh, V., Grigoriev, A., Hansen, G., Hirsh, H., Khatuntsev, I., Kiselev, A., Ignatiev, N., Jurewicz, A., Lellouch, E., Lopez Moreno, J., Marten, A., Mattana, A., Maturilli, A., Mencarelli, E., Michalska, M., Moroz, V., Moshkin, B., Nespoli, F., Nikolsky, Y., Orfei, R., Orleanski, P., Orofino, V., Palomba, E., Patsaev, D., Piccioni, G., Rataj, M., Rodrigo, R., Rodriguez, J., Rossi, M., Saggin, B., Titov, D., and Zasova, L.

Published
2005
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45. Influence of solar-related effects and topography on the cloud top circulation above Aphrodite Terra from VMC/Venus Express wind fields

Author

Patsaeva, M. V., Khatuntsev, I. V., Zasova, L. V., Hauchecorne, Alain, Titov, D.V., Bertaux, Jean-Loup, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), STRATO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), and PLANETO - LATMOS

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; A set of UV (365 nm) images obtained by the Venus Monitoring Camera [3] onboard ESA's Venus Express orbiter from 2006 to 2013 was used to study the circulation of the mesosphere. It was found that the surface topography influences on the behavior of the horizontal flow above Aphrodite Terra to at least 30°S. A maximum deceleration of the mean zonal flow is observed at noon above Ovda Regio (the highest region of Aphrodite Terra). We attributed the observed wind deceleration to interaction of the gravity (mountain) waves generated by Aphrodite Terra with the atmospheric circulation. The mean zonal and meridional flows at cloud top level in the equatorial region are perturbed by a solar tide at 13-14 h.

Published
2019

46. Planetary Fourier spectrometer: An interferometer for atmospheric studies on board Mars 94 mission

Author

Formisano, V., Moroz, V., Amata, E., Baldetti, P., Bellucci, G., Chionchio, G., Matteuzzi, A., Orfei, R., Piccioni, G., Carusi, A., Coradini, A., Cerroni, P., Capaccioni, F., Adriani, A., Viterbini, M., Angrilli, F., Baglioni, P., Bianchini, G., Fanti, G., Bussoletti, E., Fonti, S., Mancini, D., Colangeli, L., Grigoriev, A., Moshkin, B., Zasova, L., Sanko, N., Nikolsky, Y., Gnedykh, V., Kiselev, A., Khatuntsev, I., Goncharov, S., Titov, D., Hirsh, H., Arnold, G., Orleansky, P., Combes, M., Michel, G., Rodrigo, R., Lopez Moreno, J. J., Rodriguez Gomez, J., and Olivares, I.

Published
1993
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47. The Atmospheric Chemistry Suite (ACS) of three spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., 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., Zasova, L. V., Zelenyi, L. M., Zorzano, M. P., Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), National Research Institute for Physical-technical and Radiotechnical Measurements (VNIIFTRI), Scientific Production Enterprise Astron Electronics, Faculty of Physics [MSU, Moscow], Lomonosov Moscow State University (MSU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Tohoku University [Sendai], Moscow Institute of Physics and Technology [Moscow] (MIPT), Catholic University of America, Vernadsky Institute of Geochemistry and Analytical Chemistry (GEOKHI), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Computer Science [Kiruna], Luleå University of Technology (LUT), Instituto Andaluz de Ciencias de la Tierra (IACT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universidad de Granada (UGR), The Open University [Milton Keynes] (OU), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Universität Bern [Bern], Facultad de Informática [Madrid], Universidad Complutense de Madrid [Madrid] (UCM), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada (UGR), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada = University of Granada (UGR), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Universität Bern [Bern] (UNIBE), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Oxford, and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
Cross-dispersion, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atmosphere, 520 Astronomy, Mars, Echelle, Fourier-spectrometer, 620 Engineering, High-resolution spectrometer, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph]
Abstract

International audience; 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−1. 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.

Published
2018

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