11 results on '"Viscardy, Sébastien"'
Search Results
2. Methane on Mars and Habitability: Challenges and Responses
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Yung, Yuk L, Chen, Pin, Nealson, Kenneth, Atreya, Sushil, Beckett, Patrick, Blank, Jennifer G, Ehlmann, Bethany, Eiler, John, Etiope, Giuseppe, Ferry, James G, Forget, Francois, Gao, Peter, Hu, Renyu, Kleinböhl, Armin, Klusman, Ronald, Lefèvre, Franck, Miller, Charles, Mischna, Michael, Mumma, Michael, Newman, Sally, Oehler, Dorothy, Okumura, Mitchio, Oremland, Ronald, Orphan, Victoria, Popa, Radu, Russell, Michael, Shen, Linhan, Lollar, Barbara Sherwood, Staehle, Robert, Stamenković, Vlada, Stolper, Daniel, Templeton, Alexis, Vandaele, Ann C, Viscardy, Sébastien, Webster, Christopher R, Wennberg, Paul O, Wong, Michael L, and Worden, John
- Subjects
Exobiology ,Extraterrestrial Environment ,Mars ,Methane ,Spectrum Analysis ,Time Factors ,CH4 ,Subsurface redox conditions ,Mars instrumentation ,Astrobiology 18 ,xxx-xxx ,Astronomical and Space Sciences ,Geochemistry ,Geology ,Astronomy & Astrophysics - Abstract
Recent measurements of methane (CH4) by the Mars Science Laboratory (MSL) now confront us with robust data that demand interpretation. Thus far, the MSL data have revealed a baseline level of CH4 (∼0.4 parts per billion by volume [ppbv]), with seasonal variations, as well as greatly enhanced spikes of CH4 with peak abundances of ∼7 ppbv. What do these CH4 revelations with drastically different abundances and temporal signatures represent in terms of interior geochemical processes, or is martian CH4 a biosignature? Discerning how CH4 generation occurs on Mars may shed light on the potential habitability of Mars. There is no evidence of life on the surface of Mars today, but microbes might reside beneath the surface. In this case, the carbon flux represented by CH4 would serve as a link between a putative subterranean biosphere on Mars and what we can measure above the surface. Alternatively, CH4 records modern geochemical activity. Here we ask the fundamental question: how active is Mars, geochemically and/or biologically? In this article, we examine geological, geochemical, and biogeochemical processes related to our overarching question. The martian atmosphere and surface are an overwhelmingly oxidizing environment, and life requires pairing of electron donors and electron acceptors, that is, redox gradients, as an essential source of energy. Therefore, a fundamental and critical question regarding the possibility of life on Mars is, "Where can we find redox gradients as energy sources for life on Mars?" Hence, regardless of the pathway that generates CH4 on Mars, the presence of CH4, a reduced species in an oxidant-rich environment, suggests the possibility of redox gradients supporting life and habitability on Mars. Recent missions such as ExoMars Trace Gas Orbiter may provide mapping of the global distribution of CH4. To discriminate between abiotic and biotic sources of CH4 on Mars, future studies should use a series of diagnostic geochemical analyses, preferably performed below the ground or at the ground/atmosphere interface, including measurements of CH4 isotopes, methane/ethane ratios, H2 gas concentration, and species such as acetic acid. Advances in the fields of Mars exploration and instrumentation will be driven, augmented, and supported by an improved understanding of atmospheric chemistry and dynamics, deep subsurface biogeochemistry, astrobiology, planetary geology, and geophysics. Future Mars exploration programs will have to expand the integration of complementary areas of expertise to generate synergistic and innovative ideas to realize breakthroughs in advancing our understanding of the potential of life and habitable conditions having existed on Mars. In this spirit, we conducted a set of interdisciplinary workshops. From this series has emerged a vision of technological, theoretical, and methodological innovations to explore the martian subsurface and to enhance spatial tracking of key volatiles, such as CH4.
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- 2018
3. Calibration of the NOMAD-UVIS data
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Willame, Yannick, Depiesse, Cédric, Mason, Jonathon P., Thomas, Ian R., Patel, Manish R., Hathi, Brijen, Leese, Mark R., Bolsée, David, Wolff, Michael J., Trompet, Loïc, Vandaele, Ann Carine, Piccialli, Arianna, Aoki, Shohei, Ristic, Bojan, Neefs, Eddy, Beeckman, Bram, Berkenbosch, Sophie, Clairquin, Roland, Mahieux, Arnaud, Pereira, Nuno, Robert, Séverine, Viscardy, Sébastien, Wilquet, Valérie, Daerden, Frank, Lopez-Moreno, José Juan, and Bellucci, Giancarlo
- Published
- 2022
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4. Unexpected increase of the deuterium to hydrogen ratio in the Venus mesosphere.
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Mahieux, Arnaud, Viscardy, Sébastien, Yelle, Roger Vincent, Hiroki Karyu, Chamberlain, Sarah, Robert, Séverine, Piccialli, Arianna, Trompet, Loïc, Erwin, Justin Tyler, Ubukata, Soma, Hiromu Nakagawa, Shungo Koyama, Maggiolo, Romain, Pereira, Nuno, Cessateur, Gaël, Willame, Yannick, and Vandaele, Ann Carine
- Abstract
This study analyzes H2O and HDO vertical profiles in the Venus mesosphere using Venus Express/Solar Occultation in the InfraRed data. The findings show increasing H2O and HDO volume mixing ratios with altitude, with the D/H ratio rising significantly from 0.025 at ~70 km to 0.24 at ~108 km. This indicates an increase from 162 to 1,519 times the Earth's ratio within 40 km. The study explores two hypotheses for these results: isotopic fractionation from photolysis of H2O over HDO or from phase change processes. The latter, involving condensation and evaporation of sulfuric acid aerosols, as suggested by previous authors [X. Zhang et al., Nat. Geosci. 3, 834-837 (2010)], aligns more closely with the rapid changes observed. Vertical transport computations for H2O, HDO, and aerosols show water vapor downwelling and aerosols upwelling. We propose a mechanism where aerosols form in the lower mesosphere due to temperatures below the water condensation threshold, leading to deuterium-enriched aerosols. These aerosols ascend, evaporate at higher temperatures, and release more HDO than H2O, which are then transported downward. Moreover, this cycle may explain the SO2 increase in the upper mesosphere observed above 80 km. The study highlights two crucial implications. First, altitude variation is critical to determining the Venus deuterium and hydrogen reservoirs. Second, the altitude-dependent increase of the D/H ratio affects H and D escape rates. The photolysis of H2O and HDO at higher altitudes releases more D, influencing long-term D/H evolution. These findings suggest that evolutionary models should incorporate altitude-dependent processes for accurate D/H fractionation predictions. [ABSTRACT FROM AUTHOR]
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- 2024
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5. Comprehensive investigation of Mars methane and organics with ExoMars/NOMAD
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Knutsen, Elise W., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M.J., Mumma, Michael J., Smith, Michael D., Vandaele, Ann Carine, Aoki, Shohei, Thomas, Ian R., Daerden, Frank, Viscardy, Sébastien, Erwin, Justin T., Trompet, Loic, Neary, Lori, Ristic, Bojan, Lopez-Valverde, Miguel Angel, Lopez-Moreno, Jose Juan, Patel, Manish R., Karatekin, Ozgur, and Bellucci, Giancarlo
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- 2021
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6. Independent confirmation of a methane spike on Mars and a source region east of Gale Crater
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Giuranna, Marco, Viscardy, Sébastien, Daerden, Frank, Neary, Lori, Etiope, Giuseppe, Oehler, Dorothy, Formisano, Vittorio, Aronica, Alessandro, Wolkenberg, Paulina, Aoki, Shohei, Cardesín-Moinelo, Alejandro, Marín-Yaseli de la Parra, Julia, Merritt, Donald, and Amoroso, Marilena
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- 2019
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7. Publisher Correction: No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations
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Korablev, Oleg, Vandaele, Ann Carine, Montmessin, Franck, Fedorova, Anna A., Trokhimovskiy, Alexander, Forget, François, Lefèvre, Franck, Daerden, Frank, Thomas, Ian R., Trompet, Loïc, Erwin, Justin T., Aoki, Shohei, Robert, Séverine, Neary, Lori, Viscardy, Sébastien, Grigoriev, Alexey V., Ignatiev, Nikolay I., Shakun, Alexey, Patrakeev, Andrey, Belyaev, Denis A., Bertaux, Jean-Loup, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Ivanov, Yuriy S., Ristic, Bojan, Mason, Jon, Willame, Yannick, Depiesse, Cédric, Hetey, Laszlo, Berkenbosch, Sophie, Clairquin, Roland, Queirolo, Claudio, Beeckman, Bram, Neefs, Eddy, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, Jose-Juan, Wilson, Colin F., Etiope, Giuseppe, Zelenyi, Lev, Svedhem, Håkan, Vago, Jorge L., and The ACS and NOMAD Science Teams
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- 2019
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8. Publisher Correction: Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter
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Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, Francesca, López-Valverde, Miguel, Villanueva, Geronimo, Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, R. Todd, Cloutis, Edward, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, Giuranna, Marco, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen, López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James, Wilquet, Valérie, Wolff, Michael J., Bellucci, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, François, Wilson, Colin F., Young, Roland, Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, NOMAD Science Team, and ACS Science Team
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- 2019
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9. No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations.
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Korablev, Oleg, Vandaele, Ann Carine, Montmessin, Franck, Fedorova, Anna A., Trokhimovskiy, Alexander, Forget, François, Lefèvre, Franck, Daerden, Frank, Thomas, Ian R., Trompet, Loïc, Erwin, Justin T., Aoki, Shohei, Robert, Séverine, Neary, Lori, Viscardy, Sébastien, Grigoriev, Alexey V., Ignatiev, Nikolay I., Shakun, Alexey, Patrakeev, Andrey, and Belyaev, Denis A.
- 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. Highly sensitive measurements of the atmosphere of Mars with the ExoMars Trace Gas Orbiter do not detect any methane over a range of latitudes in both hemispheres, in contrast to previous local or remote detections. [ABSTRACT FROM AUTHOR]
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- 2019
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10. Ground-based infrared mapping of H2O2 on Mars near opposition.
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Encrenaz, Therese, Geathouse, Thomas, Aoki, Shohei, Daerden, Frank, Giuranna, Marco, Lefèvre, Franck, Montmessin, Franck, Forget, François, Fouchet, Thierry, Bézard, Bruno, Atreya, Sushil, DeWitt, Curtis, Richter, Matthew, Neary, Lori, and Viscardy, Sébastien
- Published
- 2019
11. Martian dust storm impact on atmospheric H 2 O and D/H observed by ExoMars Trace Gas Orbiter.
- Author
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Vandaele AC, Korablev O, Daerden F, Aoki S, Thomas IR, Altieri F, López-Valverde M, Villanueva G, Liuzzi G, Smith MD, Erwin JT, Trompet L, Fedorova AA, Montmessin F, Trokhimovskiy A, Belyaev DA, Ignatiev NI, Luginin M, Olsen KS, Baggio L, Alday J, Bertaux JL, Betsis D, Bolsée D, Clancy RT, Cloutis E, Depiesse C, Funke B, Garcia-Comas M, Gérard JC, Giuranna M, Gonzalez-Galindo F, Grigoriev AV, Ivanov YS, Kaminski J, Karatekin O, Lefèvre F, Lewis S, López-Puertas M, Mahieux A, Maslov I, Mason J, Mumma MJ, Neary L, Neefs E, Patrakeev A, Patsaev D, Ristic B, Robert S, Schmidt F, Shakun A, Teanby NA, Viscardy S, Willame Y, Whiteway J, Wilquet V, Wolff MJ, Bellucci G, Patel MR, López-Moreno JJ, Forget F, Wilson CF, Svedhem H, Vago JL, and Rodionov D
- Abstract
Global dust storms on Mars are rare
1,2 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/H2 O 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 H2 O 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 H2 O 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.- Published
- 2019
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