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81 results on '"Gonzalez-Galindo, Francisco"'

1. 3D Global climate model of an exo-Venus: a modern Venus-like atmosphere for the nearby super-Earth LP 890-9 c

Author

Quirino, Diogo, Gilli, Gabriella, Kaltenegger, Lisa, Navarro, Thomas, Fauchez, Thomas J., Turbet, Martin, Leconte, Jérémy, Lebonnois, Sébastien, and González-Galindo, Francisco

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract

The recently discovered super-Earth LP 890-9 c is an intriguing target for atmospheric studies as it transits a nearby, low-activity late-type M-dwarf star at the inner edge of the Habitable Zone. Its position at the runaway greenhouse limit makes it a natural laboratory to study the climate evolution of hot rocky planets. We present the first 3D-GCM exo-Venus model for a modern Venus-like atmosphere (92 bar surface pressure, realistic composition, H$_2$SO$_4$ radiatively-active clouds), applied to the tidally-locked LP 890-9c to inform observations by JWST and future instruments. If LP 890-9 c has developed into a modern exo-Venus, then the modelled temperatures suggest that H$_2$SO$_4$ clouds are possible even in the substellar region. Like on modern Venus, clouds on LP 890-9 c would create a flat spectrum. The strongest CO$_2$ bands in transmission predicted by our model for LP 890-9 c are about 10 ppm, challenging detection, given JWST estimated noise floor. Estimated phase curve amplitudes are 0.9 and 2.4 ppm for continuum and CO$_2$ bands, respectively. While pointing out the challenge to characterise modern exo-Venus analogues, these results provide new insights for JWST proposals and highlight the influence of clouds in the spectrum of hot rocky exoplanet spectra., Comment: 6 pages, 4 figures, MNRAS letter

Published
2023
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3. Ariel: Enabling planetary science across light-years

Author

Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Da Peppo, Vania, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Di Giorgio, Anna, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Van Eylen, Vincent, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Van der Swaelmen, Mathieu, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Del Vecchio, Ciro, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, and Zuppella, Paola

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution., Comment: Ariel Definition Study Report, 147 pages. Reviewed by ESA Science Advisory Structure in November 2020. Original document available at: https://www.cosmos.esa.int/documents/1783156/3267291/Ariel_RedBook_Nov2020.pdf/

Published
2021

7. Cooling of the Martian thermosphere by CO$_2$ radiation and gravity waves: An intercomparison study with two general circulation models

Author

Medvedev, Alexander S., González-Galindo, Francisco, Yiğit, Erdal, Feofilov, Artem G., Forget, François, and Hartogh, Paul

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics, Physics - Fluid Dynamics, Physics - Space Physics
Abstract

Observations show that the lower thermosphere of Mars ($\sim$100--140 km) is up to 40 K colder than the current general circulation models (GCMs) can reproduce. Possible candidates for physical processes missing in the models are larger abundances of atomic oxygen facilitating stronger CO$_2$ radiative cooling, and thermal effects of gravity waves. Using two state-of-the-art Martian GCMs, the Laboratoire de M\'et\'eorologie Dynamique and Max Planck Institute models that self-consistently cover the atmosphere from the surface to the thermosphere, these physical mechanisms are investigated. Simulations demonstrate that the CO$_2$ radiative cooling with a sufficiently large atomic oxygen abundance, and the gravity wave-induced cooling can alone result in up to 40 K colder temperature in the lower thermosphere. Accounting for both mechanisms produce stronger cooling at high latitudes. However, radiative cooling effects peak above the mesopause, while gravity wave cooling rates continuously increase with height. Although both mechanisms act simultaneously, these peculiarities could help to further quantify their relative contributions from future observations., Comment: Accepted for publication in Journal of Geophysical Research - Planets

Published
2015

8. The Climatology of Mars Thermospheric Polar Warming at Aphelion

Author

Thiemann, Edward M. B., primary, Trompet, Loïc, additional, Bougher, Stephen W., additional, Yiğit, Erdal, additional, Gasperini, Federico, additional, Montabone, Luca, additional, Gonzalez‐Galindo, Francisco, additional, Eparvier, Francis G., additional, and Vandaele, Anne‐Carine, additional

Published
2024
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9. Temporal Variability of Waves at the Proton Cyclotron Frequency Upstream from Mars: Implications for Mars Distant Hydrogen Exosphere

Author

Bertucci, Cesar, Romanelli, Norberto, Chaufray, Jean-Yves, Gomez, Daniel, Mazelle, Christian, Delva, Magda, Modolo, Ronan, Gonzalez-Galindo, Francisco, and Brain, David Andrew

Subjects
Physics - Space Physics
Abstract

We report on the temporal variability of the occurrence of waves at the local proton cyclotron frequency upstream from the Martian bow shock from Mars Global Surveyor observations during the first aerobraking and science phasing orbit periods. Observations at high southern latitudes during minimum-to-mean solar activity show that the wave occurrence rate is significantly higher around perihelion southern summer solstice and lower around the same hemisphere's spring and autumn equinoxes. A similar trend is observed in the hydrogen (H) exospheric density profiles over the Martian South Pole obtained from a model including UV thermospheric heating effects. In spite of the complexity in the ion pick-up and plasma wave generation and evolution processes, these results support the idea that variations in the occurrence of waves could be used to study the temporal evolution of the distant Martian H corona and its coupling with the thermosphere at altitudes currently inaccessible to direct measurements., Comment: 16 pages, 2 figures, Submitted to Geophysical Research Letters

Published
2013
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10. Modeling the Martian HDO cycle with a Global Climate Model during the “dusty” season

Author

Vals, Margaux, primary, Montmessin, Franck, additional, Rossi, Loïc, additional, Braude, Ashwin, additional, Lefèvre, Franck, additional, Gonzalez-Galindo, Francisco, additional, Chaufray, Jean-Yves, additional, Fedorova, Anna, additional, Alday, Juan, additional, Forget, François, additional, Millour, Ehouarn, additional, Korablev, Oleg, additional, Trokhimovskiy, Alexander, additional, and Shakun, Alexey, additional

Published
2022
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12. Simulation of the atomic deuterium density and escape at Mars and comparison with MAVEN/IUVS observations

Author

Chaufray, Jean-Yves, primary, Gonzalez-Galindo, Francisco, additional, Vals, Margaux, additional, Rossi, Loic, additional, Montmessin, Franck, additional, Lefevre, Franck, additional, Leblanc, François, additional, Modolo, Ronan, additional, Forget, François, additional, Millour, Ehouarn, additional, Gilli, Gabriella, additional, Lopez-Valverde, Miguel, additional, and Mayyasi, Majd, additional

Published
2022
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13. Mars water vapor vertical distributions from the troposphere to the mesosphere from NOMAD Solar Occultation for Martian Years 34 and 35

Author

Brines, Adrian, primary, Lopez Valverde, Miguel Ángel, additional, Stolzenbach, Aurélien, additional, Modak, Ashim, additional, Funke, Bernd, additional, Gonzalez Galindo, Francisco, additional, Lopez Moreno, Jose Juan, additional, Aoki, Shohei, additional, Vandaele, Ann Carine, additional, Daerden, Frank, additional, Thomas, Ian, additional, Erwin, Justin, additional, Trompet, Loïc, additional, Ristic, Bojan, additional, Villanueva, Gerónimo Luis, additional, Liuzzi, Giuliano, additional, Patel, Manish, additional, and Bellucci, Giancarlo, additional

Published
2022
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14. Vertical distribution of atmospheric temperature and density from the solar occultation instruments NOMAD and ACS on board the Trace Gas Orbiter

Author

Lopez-Valverde, Miguel Angel, primary, Funke, Bernd, additional, Brines, Adrian, additional, Stolzenbach, Aurélien, additional, Modak, Ashimananda, additional, Gonzalez-Galindo, Francisco, additional, Aoki, Shohei, additional, Trompet, Loic, additional, Thomas, Ian, additional, Villanueva, Gerónimo, additional, Liuzzi, Giuliano, additional, Belyaev, Denis, additional, Olsen, Kevin, additional, Trokhimovsky, Alexander, additional, Lopez-Moreno, Jose Juan, additional, Vandaele, Ann Carine, additional, Patel, Manish, additional, Bellucci, Giancarlo, additional, Korablev, Oleg, additional, and Montmessin, Franck, additional

Published
2022
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15. Mapping of Martian CO from NOMAD solar occultation measurements for MY35 and 36

Author

Modak, Ashimananda, primary, Lopez-Valverde, Miguel-Angel, additional, Brines, Adrian, additional, Stolzenbach, Aurelien, additional, Funke, Bernd, additional, Gonzalez-Galindo, Francisco, additional, Lopez-Moreno, Jose-Juan, additional, Aoki, Shohe, additional, Villanueva, Geronimo, additional, Liuzzi, Giuliano, additional, Bellucci, Giancarlo, additional, Yoshida, Nao, additional, Erwin, Justin, additional, Trompet, Loic, additional, Thomas, Ian, additional, Daerden, Frank, additional, Ristic, Bojan, additional, Patel, Manish, additional, Vandaele, Ann Carine, additional, and Montmessin, Franck, additional

Published
2022
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16. The HDO Cycle on Mars: Comparison of ACS Observations With GCM Simulations

Author

Rossi, Loïc, primary, Vals, Margaux, additional, Alday, Juan, additional, Montmessin, Franck, additional, Fedorova, Anna, additional, Trokhimovskiy, Alexander, additional, Korablev, Oleg, additional, Lefèvre, Franck, additional, Gonzalez‐Galindo, Francisco, additional, Luginin, Mikhail, additional, Bierjon, Antoine, additional, Forget, François, additional, and Millour, Ehouarn, additional

Published
2022
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17. Improved Modeling of Mars' HDO Cycle Using a Mars' Global Climate Model

Author

Vals, Margaux, primary, Rossi, Loïc, additional, Montmessin, Franck, additional, Lefèvre, Franck, additional, Gonzalez‐Galindo, Francisco, additional, Fedorova, Anna, additional, Luginin, Mikhail, additional, Forget, François, additional, Millour, Ehouarn, additional, Korablev, Oleg, additional, Trokhimovskiy, Alexander, additional, Shakun, Alexey, additional, Bierjon, Antoine, additional, and Montabone, Luca, additional

Published
2022
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18. Global Troposphere-to-Mesosphere Modelling of Martian CO2 Ice Clouds

Author

Määttänen, Anni, Mathé, Christophe, Audouard, Joachim, Listowski, Constantino, Millour, Ehouarn, Forget, François, Gonzalez-Galindo, Francisco, Falletti, Lola, Bardet, Déborah, Teinturier, L., Vals, Margaux, Spiga, Aymeric, Montmessin, Franck, PLANETO - 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), 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), WPO Paris, DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physics and Astronomy [Leicester], University of Leicester, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and ANR-18-CE31-0013,MECCOM,Modéliser des nuages exotiques de CO2 sur Mars(2018)

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

International audience

Published
2022

19. Publisher Correction: Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author

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

Published
2019
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20. Modeling the HDO Cycle with a Global Climate Model During the MY34 'Dusty' Season

Author

Vals, Margaux, Rossi, Loïc, Montmessin, Franck, Lefèvre, Franck, Gonzalez-Galindo, Francisco, Fedorova, Anna A., Luginin, Mikhail, Forget, François, Millour, Ehouarn, Korablev, Oleg I., Trokhimovskiy, Alexander V., Shakun, Alexey, Bierjon, Antoine, Montabone, Luca, and Cardon, Catherine

Subjects
[SDU] Sciences of the Universe [physics]
Published
2022

21. Diurnal Thermal Structure of the Martian Atmosphere from MAVEN/IUVS Stellar Occultations

Author

Gupta, Sumedha, Yelle, Roger, Mccord Schneider, Nicholas, Jain, Sonal, Gonzalez-Galindo, Francisco, Verdier, Loïc, Braude, Ashwin, Montmessin, Franck, Mayyasi, Majd, Deighan, Justin, and Cardon, Catherine

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

Recent Mars missions have provided a wealth of observations to study the red planet and its relationship to Earth. However, only few observations of Martian upper mesosphere/lower thermosphere (~80 – 160 km) are available, a region that includes the mesopause and homopause, and is closely coupled to the atmospheric layers above and below. The existing datasets in this altitude range provide only limited temporal and spatial coverage. Stellar occultations by the Imaging Ultraviolet Spectrograph (IUVS) aboard the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) mission are being designed and executed in dedicated bimonthly campaigns for the last seven years to fill this observation gap. However, only the nightside observations are useable as the current data-reduction pipeline rejects any dayside occultation with stray light contamination.We have devised an improved stray light removal algorithm to process the daytime observations as well. Of the 3003 observations from March 2015 to January 2022, the reprocessed data includes 1145 dayside and 1259 nightside events, thereby resulting in the first Martian dataset that consistently measures both the dayside and the nightside mesosphere. We present the results of the study of diurnal thermal structure in ~80 – 160 km altitude range (10-6 to 10-2 Pa).The dayside is observed to be warmer than the nightside at all pressure levels, with the diurnal variations of ~30 K in the lower thermosphere, ~20 K near the mesopause, and little day/night differences at low altitudes. This is found to be consistent with short radiative time constant of the order of 1 sol, suggesting strong tidal damping. The data also shows that the regions at pressures less than 2x10-3 Pa are under strong solar control with no prominent migrating tidal signatures. Whereas, on Earth, the temperature variations due to tides are quite large near the mesopause, with radiative time constant of ~10 Earth days. The Mars Climate Database shows an opposite diurnal trend in the mesosphere, with the dayside mesopause cooler than the nightside, along with signatures of a vertically propagating tide. The IUVS dataset provides an unprecedented constraint on the structure of the Martian mesosphere. The inconsistencies with the data imply that we do not really understand the dynamics and structure of this important region.

Published
2022

23. Simulation of the H Escape Variability with a Global Climate Model

Author

Gonzalez-Galindo, Francisco, Chaufray, Jean-Yves, Gilli, G., Brines, A., Lopez-Valverde, Miguel, Lefèvre, Franck, Vals, Margaux, Montmessin, Franck, Rossi, Loïc, Forget, Francois, Millour, Ehouarn, and Cardon, Catherine

Subjects
[SDU] Sciences of the Universe [physics]
Published
2022

26. Retrieval of Martian CO vertical profiles from NOMAD solar occultation measurements

Author

Modak, Ashimananda, primary, Lopez-Valverde, Miguel Angel, additional, Funke, Bernd, additional, Hill, Brittany, additional, Brines, Adrian, additional, Stolzenbach, Aurelien, additional, Gonzalez-Galindo, Francisco, additional, Lopez Moreno, Jose Juan, additional, Erwin, Justin, additional, Trompet, Loic, additional, Thomas, Ian, additional, Daerden, Frank, additional, Vandaele, Ann Carine, additional, Ristic, Bojan, additional, Villanueva, Geronimo, additional, Liuzzi, Giuliano, additional, Bellucci, Giancarlo, additional, and Patel, Manish, additional

Published
2021
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28. Ariel: Enabling planetary science across light-years

Author

Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Peppo, Vania Da, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Giorgio, Anna Di, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Eylen, Vincent Van, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Swaelmen, Mathieu Van der, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Vecchio, Ciro Del, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, Zuppella, Paola, Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Peppo, Vania Da, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Giorgio, Anna Di, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Eylen, Vincent Van, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Swaelmen, Mathieu Van der, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Vecchio, Ciro Del, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, and Zuppella, Paola

Abstract

The concept of a mission devoted to atmospheric characterization of exoplanets through transit spectroscopy was first considered in Europe in 2007, shortly after the DARWIN proposal submitted to ESA for the first Cosmic Vision call for L-class missions was rejected because of the need for further scientific and technical developments. Following the decision, both ESA (EP-RAT panel report, October 2010) and the Exoplanetary Community (Blue Dot Team – Barcelona conference, September 2009) started a discussion to define a roadmap for exoplanetary research. Both groups concluded that an intermediate step was needed, both scientifically and technically, before the characterisation of Earth-like planets could be tackled, and recommended a transit spectroscopy mission as a first step to atmospheric characterisation. A short study was undertaken at ESTEC in the context of the ExoPlanet Roadmap Advisory Team mandate under the name ESM (Exoplanet Spectroscopy Mission). Following this study the Exoplanet Characterisation Observatory (EChO) was proposed and accepted for assessment phase study in the context of the ESA Cosmic Vision 2015-2025 programme M3 medium class mission opportunity. Although eventually not selected, the EChO study1 allowed further development of the technical building blocks and the science case for an eventual transit spectroscopy mission. In response to the call for the next medium class opportunity, Cosmic Vision M4, a proposal was submitted in January 2015: the Atmospheric Remote-sensing InfraRed Large-survey (ARIEL). The mission was one of the three selected in June 2015 for study in a Phase 0/A, a competitive assessment phase2. ARIEL was eventually selected as M4 in March 2018, and went into Phase B1, the definition study phase. The name of the mission has been changed to Ariel after selection. During Phase B1, the science case was studied in depth and consolidated under auspices of the Science Advisory Team, the bulk of the work be

Published
2020

29. CO2 and temperature retrievals in the Mars atmosphere from solar occultation by NOMAD-SO and ACS-MIR: performance and cross validation.

Author

Lopez-Valverde, Miguel Angel, primary, Funke, Bernd, additional, Hill, Brittany, additional, Gonzalez-Galindo, Francisco, additional, Aoki, Shohei, additional, Trompet, Loic, additional, Thomas, Ian, additional, Villanueva, Geronimo, additional, Erwin, Justin, additional, Olsen, Kevin, additional, Belyaev, Denis, additional, Trokhimovskiy, Alexander, additional, Alday Parejo, Juan, additional, Lopez-Puertas, Manuel, additional, Lopez-Moreno, Jose Juan, additional, Montmessin, Franck, additional, Patel, Manish, additional, Bellucci, Giancarlo, additional, Vandele, Ann Carine, additional, and Korablev, Oleg, additional

Published
2020
Full Text
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30. Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author

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., Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, NOMAD Science Team, Alonso-Rodrigo, Gustavo, Bauduin, Sophie, Carrozzo, Giacomo, Crismani, Matteo, da Pieve, Fabiana, D'AVERSA, EMILIANO, Etiope, Giuseppe, Fussen, Didier, Geminale, Anna, Gkouvelis, Leo, Holmes, James, Hubert, Benoît, Ignatiev, Nicolay I., Kasaba, Yasumasa, Kass, David, Kleinböhl, Armin, LANCIANO, ORIETTA, Nakagawa, Hiromu, Novak, Robert E., Oliva, Fabrizio, Piccialli, Arianna, Renotte, Etienne, Ritter, Birgit, Schneider, Nick, SINDONI, Giuseppe, Thiemann, Ed, Vander Auwera, Jean, Wilquet, Valerie, WOLKENBERG, PAULINA MARIA, Yelle, Roger, ACS Science Team, Anufreychik, Konstantin, Arnold, Gabriele, Duxbury, Natalia, Fouchet, Thierry, GRASSI, Davide, Guerlet, Sandrine, Hartogh, Paul, Khatuntsev, Igor, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, Lellouch, Emmanuel, Määttänen, Anni, Marcq, Emmanuel, Martin-Torres, Javier, Medvedev, Alexander, Millour, Ehouarn, Moshkin, Boris, Quantin-Nataf, Cathy, Rodin, Alexander, Shematovich, Valery, Thomas, Nicolas, Trokhimovsky, Alexander, Vazquez, Luis, Vincendon, Matthieu, Young, Roland, Zasova, Ludmila, Zelenyi, Lev, Zorzano, Maria Paz, Parejo, J, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, NASA Goddard Space Flight Center (GSFC), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Agenzia Spaziale Italiana (ASI), Graduate School of Information Sciences [Sendai], Tohoku University [Sendai], Advanced Mechanical and Optical Systems SA (AMOS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], School of Earth Sciences [Bristol], University of Bristol [Bristol], Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Department of Physics [Oxford], University of Oxford [Oxford], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), PLANETO - 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), Lomonosov Moscow State University (MSU), 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), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Institute for Astrophysics and Computational Sciences [Washington], Catholic University of America, Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), 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), Moscow Institute of Physics and Technology [Moscow] (MIPT), Institute of Astronomy of the Russian Academy of Sciences (INASAN), University of Bern, Universidad Complutense de Madrid = Complutense University of 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), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Libre de Bruxelles [Bruxelles] (ULB), The Open University [Milton Keynes] (OU), Polska Akademia Nauk (PAN), Royal Observatory of Belgium [Brussels], IMPEC - 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS 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), Universidad Complutense de Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, 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), 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), 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), and Russian Government

Subjects
Martian, Ice cloud, Multidisciplinary, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Storm, Atmosphere of Mars, Atmospheric sciences, 01 natural sciences, Trace gas, chemistry.chemical_compound, chemistry, 13. Climate action, Dust storm, 0103 physical sciences, Environmental science, Semiheavy water, 010303 astronomy & astrophysics, Water vapor, 0105 earth and related environmental sciences, Sciences exactes et naturelles
Abstract

A publisher correction to this article was published on 17 April 2019, 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., This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493); by the Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER); by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1; and the Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique - FNRS under grant number 30442502 (ET_HOME). The ACS experiment is led by IKI, Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government.

Published
2019
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31. No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations

Author

Korablev, Oleg, Avandaele, Ann Carine, Montmessin, Franck, Fedorova, Anna A., Trokhimovskiy, Alexander, Forget, François, Lefèvre, Franck, Daerden, Frank, Thomas, Ian R., Trompet, Loïc, Erwin, Justin T., Kasaba, Yasumasa, Kass, David, Khatuntsev, Igor, Kleinböhl, Armin, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, LANCIANO, ORIETTA, Lellouch, Emmanuel, Oliva, Fabrizio, Lewis, Stephen, Luginin, Mikhail, Liuzzi, Giuliano, López-Puertas, Manuel, López-Valverde, Miguel, Määttänen, Anni, Mahieux, Arnaud, Marcq, Emmanuel, Martin-Torres, Javier, Maslov, Igor, Patsaev, Dmitry, Medvedev, Alexander, Millour, Ehouarn, Moshkin, Boris, Mumma, Michael J., Nakagawa, Hiromu, Novak, Robert E., Piccialli, Arianna, Quantin-Nataf, Cathy, Renotte, Etienne, Ritter, Birgit, Rodin, Alexander, Schmidt, Frédéric, Schneider, Nick, Shematovich, Valery, Aoki, Shohei, Smith, Michael D., Teanby, Nicholas A., Thiemann, Ed, Thomas, Nicolas, Vander Auwera, Jean, Vazquez, Luis, Villanueva, Geronimo, Vincendon, Matthieu, Whiteway, James, Wilquet, Valérie, Robert, Séverine, Wolff, Michael J., WOLKENBERG, PAULINA MARIA, Yelle, Roger, Young, Roland, Zasova, Ludmila, Zorzano, Maria Paz, 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., ACS Science Team, NOMAD Science Team, Alonso-Rodrigo, Gustavo, ALTIERI, FRANCESCA, Anufreychik, Konstantin, Arnold, Gabriele, Bauduin, Sophie, Bolsée, David, CARROZZO, FILIPPO GIACOMO, Clancy, R. Todd, CLOUTIS, EDWARD, Crismani, Matteo, da Pieve, Fabiana, D'AVERSA, EMILIANO, Duxbury, Natalia, Encrenaz, Therese, Fouchet, Thierry, Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Gérard, Jean-Claude, GIURANNA, MARCO, Gkouvelis, Leo, Gonzalez-Galindo, Francisco, GRASSI, Davide, Guerlet, Sandrine, Hartogh, Paul, Holmes, James, Hubert, Benoît, Kaminski, Jacek, Karatekin, Ozgur, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), PLANETO - 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), 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), 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), Department of Physics [Oxford], University of Oxford [Oxford], Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Roma (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Faculty of Environmental Science and Engineering [Cluj-Napoca], Babes-Bolyai University [Cluj-Napoca] (UBB), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, NASA Goddard Space Flight Center (GSFC), Lomonosov Moscow State University (MSU), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Graduate School of Information Sciences [Sendai], Tohoku University [Sendai], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institute for Astrophysics and Computational Sciences [Washington], Catholic University of America, Agenzia Spaziale Italiana (ASI), Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), 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), Advanced Mechanical and Optical Systems SA (AMOS), Moscow Institute of Physics and Technology [Moscow] (MIPT), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Institute of Astronomy of the Russian Academy of Sciences (INASAN), School of Earth Sciences [Bristol], University of Bristol [Bristol], University of Bern, Universidad Complutense de Madrid = Complutense University of 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), Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, 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, IMPEC - 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), The Open University [Milton Keynes] (OU), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Libre de Bruxelles [Bruxelles] (ULB), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Polska Akademia Nauk (PAN), Royal Observatory of Belgium [Brussels], Universidad Complutense de Madrid [Madrid] (UCM), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), University of Oxford, Agence Spatiale Européenne = European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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), and 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)

Subjects
Martian, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Chemistry, Atmosphere of Mars, Mars Exploration Program, 01 natural sciences, 7. Clean energy, Methane, Trace gas, law.invention, Astrobiology, Atmosphere, Orbiter, chemistry.chemical_compound, 13. Climate action, law, Atmospheric chemistry, 0103 physical sciences, 010303 astronomy & astrophysics, Sciences exactes et naturelles, 0105 earth and related environmental sciences
Abstract

A publisher correction to this article was published on 17 April 2019, 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., ExoMars is the space mission of ESA and Roscosmos. The ACS experiment is led by IKI, the Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (BIRA-IASB), assisted by co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the UK (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination of the ESA Prodex Office (PEA 4000103401 and PEA 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER), as well as by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1, and the Italian Space Agency through grant 2018-2-HH.0. This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant number 30442502 (ET_HOME).

Published
2019
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32. Methane on Mars: New insights into the sensitivity of CH4 with the NOMAD/ExoMars spectrometer through its first in flight calibration

Author

Liuzzi, Giuliano, Villanueva, Geronimo L., Mumma, Michael J., Smith, Michael D., Daerden, Frank, Ristic, Bojan, Thomas, Ian R., Vandaele, Ann Carine, Patel, Manish R., Lopez-Moreno, José-Juan, Bellucci, Giancarlo, Allen, M., Alonso-Rodrigo, G., Altieri, Francesca, Aoki, Shohei, Bauduin, Sophie, Bolsée, David, Clancy, Todd, Cloutis, Edward, D'Aversa, Emiliano, Depiesse, Cédric, Erwin, Justin T., Fedorova, Anna A., Formisano, V., Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez-Galindo, Francisco, Hewson, Will, Holmes, James, Ignatiev, Nikolay I., Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Y., Lanciano, Orietta, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, López-Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mc Connell, Jack, Nakagawa, Hiromu, Neary, Lori, Neefs, Eddy, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Robert, Séverine, Sindoni, G., Stiepen, A., Trokhimovskiy, Alexander, Vander Auwera, Jean, Viscardy, Sébastien, Whiteway, James J.A., Willame, Yannick, Wilquet, Valérie, Wolff, Michael J., Wolkenberg, Paulina, Aparicio del Moral, Beatriz, Barzin, Pascal, Beeckman, Bram, BenMoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, S., Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Hathi, Brijen, Jeronimo, Zafra, Leese, M., Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, José., Morales, Rafael, Orban, Anne, Pastor-Morales, M., Perez-grande, Isabel, Queirolo, Claudio, Gómez-Rodriguez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan-Felipe, Thibert, Tanguy, Liuzzi, Giuliano, Villanueva, Geronimo L., Mumma, Michael J., Smith, Michael D., Daerden, Frank, Ristic, Bojan, Thomas, Ian R., Vandaele, Ann Carine, Patel, Manish R., Lopez-Moreno, José-Juan, Bellucci, Giancarlo, Allen, M., Alonso-Rodrigo, G., Altieri, Francesca, Aoki, Shohei, Bauduin, Sophie, Bolsée, David, Clancy, Todd, Cloutis, Edward, D'Aversa, Emiliano, Depiesse, Cédric, Erwin, Justin T., Fedorova, Anna A., Formisano, V., Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez-Galindo, Francisco, Hewson, Will, Holmes, James, Ignatiev, Nikolay I., Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Y., Lanciano, Orietta, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, López-Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mc Connell, Jack, Nakagawa, Hiromu, Neary, Lori, Neefs, Eddy, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Robert, Séverine, Sindoni, G., Stiepen, A., Trokhimovskiy, Alexander, Vander Auwera, Jean, Viscardy, Sébastien, Whiteway, James J.A., Willame, Yannick, Wilquet, Valérie, Wolff, Michael J., Wolkenberg, Paulina, Aparicio del Moral, Beatriz, Barzin, Pascal, Beeckman, Bram, BenMoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, S., Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Hathi, Brijen, Jeronimo, Zafra, Leese, M., Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, José., Morales, Rafael, Orban, Anne, Pastor-Morales, M., Perez-grande, Isabel, Queirolo, Claudio, Gómez-Rodriguez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan-Felipe, and Thibert, Tanguy

Abstract

info:eu-repo/semantics/published

Published
2019

33. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD

Author

Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, Loïc, Robert, S., Neary, Lori, Viscardy, Sébastien, Clancy, Todd, Smith, Michael D., López-Valverde, Miguel, Hill, B., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, Jose-Juan, Alonso-Rodrigo, G., Altieri, F., Bauduin, Sophie, Bolsée, D., Carrozzo, Giacomo, Cloutis, Edward, Crismani, Matteo, Da Pieve, Fabiana, D'Aversa, Emiliano, Depiesse, Cédric, Etiope, Giuseppe, Fedorova, Anna A., Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Geminale, A., Gérard, Jean-Claude, Giuranna, Marco, Gkouvelis, Leo, Gonzalez-Galindo, Francisco, Holmes, James, Hubert, B., Ignatiev, Nikolay I., Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Y., Kass, David, Kleinböhl, A., Lanciano, Orietta, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, Mahieux, Arnaud, Mason, Jon, Mege, Daniel, Mumma, Michael J., Nakagawa, Hiromu, Neefs, Eddy, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Ritter, Birgit, Robert, Séverine, Schmidt, Frédéric, Schneider, N., Sindoni, G., Teanby, Nicholas A., Thiemann, Ed, Trokhimovskiy, Alexander, Vander Auwera, Jean, Whiteway, James J.A., Wilquet, Valérie, Willame, Yannick, Wolff, Michael J., Wolkenberg, Paulina, Yelle, R., Aparicio del Moral, Beatriz, Barzin, Pascal, Beeckman, Bram, BenMoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, S., Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Hathi, Brijen, Jeronimo, Zafra, Leese, M., Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, José., Morales, Rafael, Orban, Anne, Pastor-Morales, M., Perez-grande, Isabel, Queirolo, Claudio, Gómez-Rodriguez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan-Felipe, Thibert, Tanguy, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, Loïc, Robert, S., Neary, Lori, Viscardy, Sébastien, Clancy, Todd, Smith, Michael D., López-Valverde, Miguel, Hill, B., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, Jose-Juan, Alonso-Rodrigo, G., Altieri, F., Bauduin, Sophie, Bolsée, D., Carrozzo, Giacomo, Cloutis, Edward, Crismani, Matteo, Da Pieve, Fabiana, D'Aversa, Emiliano, Depiesse, Cédric, Etiope, Giuseppe, Fedorova, Anna A., Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Geminale, A., Gérard, Jean-Claude, Giuranna, Marco, Gkouvelis, Leo, Gonzalez-Galindo, Francisco, Holmes, James, Hubert, B., Ignatiev, Nikolay I., Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Y., Kass, David, Kleinböhl, A., Lanciano, Orietta, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, Mahieux, Arnaud, Mason, Jon, Mege, Daniel, Mumma, Michael J., Nakagawa, Hiromu, Neefs, Eddy, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Ritter, Birgit, Robert, Séverine, Schmidt, Frédéric, Schneider, N., Sindoni, G., Teanby, Nicholas A., Thiemann, Ed, Trokhimovskiy, Alexander, Vander Auwera, Jean, Whiteway, James J.A., Wilquet, Valérie, Willame, Yannick, Wolff, Michael J., Wolkenberg, Paulina, Yelle, R., Aparicio del Moral, Beatriz, Barzin, Pascal, Beeckman, Bram, BenMoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, S., Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Hathi, Brijen, Jeronimo, Zafra, Leese, M., Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, José., Morales, Rafael, Orban, Anne, Pastor-Morales, M., Perez-grande, Isabel, Queirolo, Claudio, Gómez-Rodriguez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan-Felipe, and Thibert, Tanguy

Abstract

info:eu-repo/semantics/published

Published
2019

34. Atmospheric and aeronomy investigations by ESA's Mars express

Author

Titov, Dmitrij V., Bibring, Jean-Pierre, Cardesin, alejandro, Duxbury, Thomas, Forget, Francois, Giuranna, Marco, Gonzalez-Galindo, Francisco, Holmström, Mats, Jaumann, Ralf, Määttänen, Anni, Martin, Patrick, Montmessin, Franck, Orosei, Roberto, Paetzold, Martin, Plaut, Jeffrey J., European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), 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), European Space Astronomy Centre (ESAC), George Mason University [Fairfax], 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), 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), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Swedish Institute of Space Physics [Kiruna] (IRF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), PLANETO - 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), Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Rhenish Institute for Environmental Research (RIU), University of Cologne, Jet Propulsion Laboratory (JPL), and NASA-California Institute of Technology (CALTECH)

Subjects
[SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Physics::Geophysics
Abstract

International audience; Mars Express remains one of ESA’s most scientifically productive missions whose publication record now exceeds 1000 papers. Characterization of the geological processes on a local-toregional scale by HRSC, OMEGA and partner experiments on NASA spacecraft has allowed constraining land-forming processes in space and time. Recent results suggest episodic geological activity as well as the presence of large bodies of liquid water in several provinces (e.g. Eridania Planum, Terra Chimeria) in the early and middle Amazonian epoch and formation of vast sedimentary plains north of the Hellas basin. Mars Express observations and experimental teams provided essential contribution to the selection of the Mars-2020 landing sites. More than a decade-long record of the atmospheric parameters such as temperature, dust loading, water vapor and ozone abundance, water ice and CO2 clouds distribution, collected by SPICAM, PFS and OMEGA spectrometers as well as subsequent modeling have provided key contributions to our understanding of the martian climate. ASPERA-3 observations of the ion escape covering complete solar cycle have revealed important dependencies of the atmospheric erosion rate on parameters of the solar wind and EUV flux. The structure of the ionosphere sounded by the MARSIS radar and the MaRS radio science experiment was found to be significantly affected by the solar activity, the crustal magnetic field, as well as by the influx of meteorite and cometary dust. MARSIS and ASPERA-3 observations suggest that the sunlit ionosphere over the regions with strong crustal fields is denser and extends to higher altitudes as compared to the regions with no crustal anomalies. The ionospheric plasma expands to higher altitudes where it contacts with the solar wind plasma. Reconnection of solar magnetic field lines carried by the solar wind with field lines of crustal origin opens channels through which the ionospheric plasma escapes to space, producing strong and narrow cavities in the density. The situation is very different on the night side where the ionosphere has patchy structure. Such patchy ionizations are observed in the regions where field lines have a dominant vertical component. Through these patches the ionospheric plasma from the dayside penetrates and supplies the nightside ionosphere. Mars Express provides unique observation capabilities amongst the flotilla of spacecraft investigating Mars. The mission has been extended till the end of 2020. The observation program proposed for 2019-2020 includes both augmenting the coverage and extending long-time series, as well as new elements and potentially new opportunities for discoveries. It will be boosted by collaboration and synergies with NASA’s MAVEN, ESA-Roscosmos Trace Gas Orbiter and other missions. The talk will give the mission status, review the recent science highlights, and outline future plans

Published
2018

36. Modeling Wind‐Driven Ionospheric Dynamo Currents at Mars: Expectations for InSight Magnetic Field Measurements

Author

Lillis, Robert J., primary, Fillingim, Matthew O., additional, Ma, Yingjuan, additional, Gonzalez‐Galindo, Francisco, additional, Forget, François, additional, Johnson, Catherine L., additional, Mittelholz, Anna, additional, Russell, Christopher T., additional, Andersson, Laila, additional, and Fowler, Christopher M., additional

Published
2019
Full Text
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37. Upper Neutral Atmosphere and Ionosphere

Author

David Brain, Stephen W. Bougher, Paul Withers, Jane L. Fox, Gonzalez-Galindo Francisco, and Cyril Simon-Wedlund

Subjects
ta115, Neutral atmosphere, Environmental science, Geophysics, Ionosphere
Published
2017
Full Text
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38. Mars Express recent findings and future plans

Author

Titov, Dmitrij V., Bibring, Jean-Pierre, Cardesin, Alejandro, Duxbury, Thomas, Forget, François, Giuranna, Marco, Gonzalez-Galindo, Francisco, Holmström, Mats, Jaumann, Ralf, Määttänen, Anni, Martin, Patrick, Montmessin, Franck, Orosei, Roberto, Pätzold, Martin, Plaut, Jeffrey J., European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), 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), European Space Astronomy Centre (ESAC), George Mason University [Fairfax], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Swedish Institute of Space Physics [Kiruna] (IRF), DLR Institute of Planetary Research, German Aerospace Center (DLR), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Radioastronomia [Bologna] (IRA), Rhenish Institute for Environmental Research (RIU), University of Cologne, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Agence Spatiale Européenne = European Space Agency (ESA), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; Mars Express remains one of ESA’s most scientifically productive missions whose publication record nowexceeds 1000 papers. Characterization of geological processes on a local-to-regional scale by HRSC, OMEGAand partner experiments on NASA spacecraft has allowed constraining land-forming processes in space and time.Recent results suggest episodic geological activity as well as the presence of large bodies of liquid water in severalprovinces (e.g. Eridania Planum, Terra Chimeria) in the early and middle Amazonian epoch and formation ofvast sedimentary plains north of the Hellas basin. Mars Express observations and experimental teams providedan essential contribution to the selection of the Mars-2020 landing sites. More than a decade-long record ofatmospheric parameters such as temperature, dust loading, water vapor and ozone abundance, water ice and CO2clouds distribution, collected by SPICAM, PFS and OMEGA spectrometers as well as subsequent modeling haveprovided key contributions to our understanding of the martian climate. The ASPERA-3 observations of ionescape covering a complete solar cycle have revealed important dependencies of the atmospheric erosion rate onparameters of the solar wind and EUV flux. Structure of the ionosphere sounded by the MARSIS radar and theMaRS radio science experiment was found to be significantly affected by the solar activity, the crustal magneticfield, as well as by the influx of meteorite and cometary dust. MARSIS and ASPERA-3 observations suggestthat the sunlit ionosphere over the regions with strong crustal fields is denser and extends to higher altitudes ascompared to the regions with no crustal anomalies. The ionospheric plasma expands to higher altitudes where itcontacts with the solar wind plasma. Reconnection of solar magnetic field lines carried by the solar wind withfield lines of crustal origin opens channels through which the ionospheric plasma escapes to space, producingstrong and narrow cavities in the density. The situation is very different on the night side where the ionosphere hasa patchy structure. Such patchy ionizations are observed in the regions where crustal field lines have a dominantvertical component. Through these patches the ionospheric plasma from the dayside penetrates and supplies thenightside ionosphere.Mars Express has fully accomplished its objectives set for 2015-2016. The mission provides unique observationcapabilities amongst the flotilla of spacecraft investigating Mars. The mission has been confirmed till the endof 2018. The science case for the mission extension until the end of 2020 has been submitted. The observationprogram proposed for 2019-2020 includes both augmenting the coverage and extending long-time series, aswell as new elements and potentially new opportunities for discoveries. It will be boosted by collaboration andsynergies with NASA’s MAVEN, ESA-Roscosmos ExoMars-2016 Trace Gas Orbiter and other missions. The talkwill give the mission status, review the recent science highlights, and outline future plans.

Published
2017

39. MARS EXPRESS: Mission Status, Recent Findings and future Plans

Author

Titov, Dmitrij V., Bibring, Jean-Pierre, Cardesin-Moinelo, A., Martin, Patrick, Duxbury, Tom, Forget, François, Giuranna, Marco, Gonzalez-Galindo, Francisco, Holmström, Mats, Jaumann, Ralf, Määttänen, Anni, Montmessin, Franck, Orosei, Roberto, Pätzold, Martin, Plaut, Jeffrey J., European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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)-Centre National d’Études Spatiales [Paris] (CNES), European Space Astronomy Centre (ESAC), George Mason University [Fairfax], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Swedish Institute of Space Physics [Kiruna] (IRF), DLR Institute of Planetary Research, German Aerospace Center (DLR), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Radioastronomia [Bologna] (IRA), Rhenish Institute for Environmental Research (RIU), University of Cologne, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Agency (ESA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; Mars Express has entered its second decade in orbit in excellent health. Characterization of geological processes and landforms on Mars on a local-to- regional scale by HRSC camera constrained the mar- tian geological activity in space and time and sug- gested its episodicity. Six years of spectro-imaging observations by OMEGA allowed correction of the surface albedo for presence of the atmospheric dust and revealed changes associated with the dust storm seasons. Imaging and spectral imaging of the surface shed light on past and present aqueous activity and contributed to the selection of the Mars-2018 landing sites. More than a decade long record of climatologi- cal parameters such as temperature, dust loading, water vapor, and ozone abundance was established by SPICAM and PFS spectrometers. Observed varia- tions of HDO/H2O ratio above the subliming North polar cap suggested seasonal fractionation. The ASPERA observations of ion escape covering a complete solar cycle revealed important dependences of the atmospheric erosion rate on parameters of the solar wind and EUV flux. Structure of the ionosphere sounded by MARSIS radar and MaRS radio science experiment was found to be significantly affected by the solar activity, crustal magnetic field as well as by influx of meteorite and cometary dust. The new atlas of Phobos based on the HRSC imaging was issued.Mars Express remains one of ESA’s most scientifi- cally productive missions and has fully accomplished its objectives set for 2015-2016. The mission pro- vides unique capabilities amongst the flotilla of spacecraft investigating Mars. The science case for the mission extension till the end of 2020 has just been submitted. The science objectives for 2017- 2018 are confirmed and fully achievable. The obser- vation programme proposed for 2019-2020 includes both augmenting the coverage and extending long- time series, as well as new elements and potentially new discoveries. It will be boosted by collaboration and synergies with NASA’s MAVEN, ESA- Roscosmos ExoMars-2016 Trace Gas Orbiter and other missions. The talk will give the mission status, review the recent science highlights, and outline fu- ture plans.

Published
2017

40. Mars’ seasonal mesospheric transport seen through nitric oxide nightglow

Author

Milby, Zachariah, Stiepen, Arnaud, Jain, Sonal, Schneider, Nicholas M., Deighan, Justin, Gonzalez-Galindo, Francisco, Gérard, Jean-Claude, Stevens, Michael H., Bougher, Stephen W., Evans, J. Scott, Stewart, A. Ian, Chaffin, Michael, Crismani, Matteo, Mcclintock, William E., Clarke, John T., Holsclaw, Greg, Montmessin, Franck, Lefèvre, Franck, Forget, Francois, Lo, Daniel Y., Hubert, Benoît, Jakosky, Bruce, Cardon, Catherine, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Naval Research Laboratory (NRL), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Computational Physics, Inc., Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), STRATO - LATMOS, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

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

International audience; We analyze the ultraviolet nightglow in the atmosphere of Mars through nitric oxide (NO) δ and γ band emissions as observed by the Imaging UltraViolet Spectrograph (IUVS) instrument onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft when it is at apoapse and periapse.In the dayside thermosphere of Mars, solar extreme-ultraviolet radiation dissociates CO2 and N2 molecules. O(3P) and N(4S) atoms are carried from the dayside to the nightside by the day-night hemispheric transport process, where they descend through the nightside mesosphere and can radiatively recombine to form NO(C2Π). The excited molecules rapidly relax by emitting photons in the UV δ and γ bands. These emissions are indicators of the N and O atom fluxes from the dayside to Mars’ nightside and the descending circulation pattern from the nightside thermosphere to the mesosphere (e.g. Bertaux et al., 2005 ; Bougher et al., 1990 ; Cox et al., 2008 ; Gagné et al., 2013 ; Gérard et al., 2008 ; Stiepen et al., 2015, 2017).Observations of these emissions are gathered from a large dataset spanning different seasonal conditions.We present discussion on the variability in the brightness and altitude of the emission with season, geographical position (longitude), and local time, along with possible interpretation by local and global changes in the mesosphere dynamics. We show the possible impact of atmospheric waves forcing longitudinal variability and data-to-model comparisons indicating a wave-3 structure in Mars’ nightside mesosphere. Quantitative comparison with calculations of the Laboratoire de Météorologie Dynamique-Mars Global Climate Model (LMD-MGCM) suggests the model reproduces both the global trend of NO nightglow emission and its seasonal variation. However, it also indicates large discrepancies, with the emission up to a factor 50 times fainter in the model, suggesting that the predicted transport is too efficient toward the night winter pole in the thermosphere by ˜20° latitude to the north.These questions are now addressed through an extensive dataset of disk images, in complement to improved simulations of the LMD-MGCM and the Mars Global Ionosphere-Thermosphere Model (MGITM) models.

Published
2017

41. Seasonal Transport in Mars’ Mesosphere-Thermosphere revealed by Nitric Oxide nightglow

Author

Stiepen, Arnaud, Royer, Emilie M., McCord Schneider, Nicholas, Jain, Sonal, Milby, Zachariah, Deighan, Justin, Gonzalez-Galindo, Francisco, Bougher, Stephen W., Gérard, Jean-Claude, Stevens, Michael H., Evans, J. Scott, Stewart, Ian F., Chaffin, Michael, Mcclintock, Bill, Clarke, John T., Montmessin, Franck, Holsclaw, Greg, Lefèvre, Franck, Forget, François, Lo, Daniel, Hubert, Benoit A., Jakosky, Bruce Martin, Cardon, Catherine, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Naval Research Laboratory (NRL), Computational Physics, Inc., Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Arizona, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

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

International audience; We analyze the ultraviolet nightglow in the atmosphere of Mars through the Nitric Oxide (NO) δ and γ band emissions observed by the Imaging Ultraviolet Spectrograph (IUVS, McClintock et al., 2015) when the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft is at apoapsis and periapsis.On the dayside thermosphere of Mars, solar extreme ultraviolet radiation dissociates CO2 and N2 molecules. O(3P) and N(4S) atoms are carried by the day-to-night hemispheric transport. They descend in the nightside mesosphere, where they can radiatively recombine to form NO(C2Π). The excited molecules rapidly relax by emitting UV photons in the δ and γ bands. These emissions are thus indicators of the N and O atom fluxes transported from the dayside to Mars’ nightside and the descending circulation pattern from the nightside thermosphere to the mesosphere (e.g. Bertaux et al., 2005 ; Bougher et al., 1990 ; Cox et al., 2008 ; Gagné et al., 2013 ; Gérard et al., 2008 ; Stiepen et al., 2015, 2017).A large dataset of nightside disk images and vertical limb scans during southern winter, fall equinox and southern summer conditions have been accumulated since the beginning of the mission.We will present a discussion regarding the variability of the brightness and altitude of the emission with season, geographical position (longitude) and local time and possible interpretation for local and global changes in the mesosphere dynamics. We show the possible impact of atmospheric waves structuring the emission longitudinally and indicating a wave-3 structure in Mars’ nightside mesosphere. Quantitative comparison with calculations from the LMD-MGCM (Laboratoire de Météorologie Dynamique-Mars Global Climate Model) show that the model globally reproduces the trends of the NO nightglow emission and its seasonal variation but also indicates large discrepancies (up to a factor 50 fainter in the model) suggesting that the predicted transport is too efficient toward the night winter pole in the thermosphere by ∼20° latitude north.These questions are now addressed with an extensive dataset of disk images, complemented with improved simulations from the LMD-MGCM and new M-GITM (Mars Global Ionosphere-Thermosphere Model) simulations of emissions for selected sampling periods.

Published
2017

42. Martian Mesospheric CO2 Clouds: a Review of a Decade of Studies

Author

Määttänen, Anni, Gondet, Brigitte, Montmessin, Franck, Hoffmann, Harald, Gonzalez-Galindo, Francisco, Spiga, Aymeric, Listowski, Constantino, Bibring, Jean-Pierre, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), DLR Institute of Planetary Research, German Aerospace Center (DLR), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; The mesospheric CO2 ice clouds were among the major discoveries of the ESA Mars Express (MEx) mission: they were detected by OMEGA [Montmessin et al., 2007, JGR 112] after clear hints from SPICAM and PFS [Montmessin et al., 2006. Icarus 183; Formisano et al., 2006. Icarus 182]. We present here a review of OMEGA and HRSC observations, compared to other datasets, and the most recent results from modeling. The cloud climatology that can be compiled from all published datasets covers nine Martian Years. It shows a clear confinement in the tropics (+/-20°N) with a distinct longitudinal distribution, and a group of midlatitude clouds observed at local autumn in both hemispheres. The first tropical clouds form around the spring equinox (Ls=330°-30°), and have a clear formation peak at the beginning of the year until just before the summer solstice. A second formation period starts some time after the solstitial pause. No equatorial cloud has been observed in the Ls=150°-330° timeframe. The equatorial daytime clouds form mostly at 60-80 km, with a particle effective radius reff of 1-3 μm and an opacity τ2 ice clouds in a global climate simulation context.

Published
2016

43. Optical and radiometric models of the NOMAD instrument part II: The infrared channels - SO and LNO

Author

Thomas, I. R., Vandaele, A. C., Robert, S., Neefs, E., Drummond, R., Daerden, F., Delanoye, S., Ristic, B., Berkenbosch, S., Clairquin, R., Maes, J., Bonnewijn, S., Depiesse, C., Mahieux, A., Trompet, L., Neary, L., Willame, Y., Wilquet, V., Nevejans, D., Aballea, L., Moelans, W., De Vos, L., Lesschaeve, S., Van Vooren, N., Lopez Moreno, J. J., Patel, M. R., Bellucci, G., Vandaele, Ann Carine, Moreno, Lopez, Juan, Jose, Bellucci, Giancarlo, Patel, Manish, Allen, Mark, Altieri, Francesca, Aoki, Shohei, Bolsée, David, Clancy, Todd, Cloutis, Edward, Daerden, Frank, Depiesse, Cédric, Fedorova, Anna, Formisano, Vittorio, Funke, Bernd, Fussen, Didier, Garcia Comas, Maya, Geminale, Anna, Gérard, Jean Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez Galindo, Francisco, Ignatiev, Nicolai, Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Yasumasa, Lefèvre, Franck, Lewis, Stephen, López Puertas, Manuel, López Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mcconnell, Jack, Mumma, Mike, Neary, Lori, Neefs, Eddy, Novak, Robert, Renotte, Etienne, Robert, Séverine, Sindoni, Giuseppe, Smith, Mike, Thomas, Ian R., Trokhimovsky, Sacha, Vander Auwera, Jean, Villanueva, Geronimo, Whiteway, Jim, Willame, Yannick, Wilquet, Valerie, Wolff, Mike, Alonso Rodrigo, Gustavo, Aparicio Del Moral, Beatriz, Barzin, Pascal, Benmoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, Sabrina, Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Delanoye, Sofie, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Zafra, Jose Jeronimo, Leese, Mark, Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, Jose, Morales, Rafael, Orban, Anne, Del Carmen Pastor Morales, Maria, Perez Grande, Isabel, Ristic, Bojan, Rodriguez Gomez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan Felipe, Thibert, Tanguy, Belgian Science Policy Office, European Space Agency, and UK Space Agency

Subjects
Physics, Martian, 010504 meteorology & atmospheric sciences, Spectrometer, Atmospheric composition, Spectrometers and spectroscopic instrumentation, 01 natural sciences, Occultation, Atomic and Molecular Physics, and Optics, Trace gas, law.invention, Remote sensing and sensors, Orbiter, Space instrumentation, Atmosphere of Earth, law, Atomic and Molecular Physics, Martian surface, 0103 physical sciences, Nadir, Radiative transfer, and Optics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract

NOMAD is a suite of three spectrometers that will be launched in 2016 as part of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument contains three channels that cover the IR and UV spectral ranges and can perform solar occultation, nadir and limb observations, to detect and map a wide variety of Martian atmospheric gases and trace species. Part I of this work described the models of the UVIS channel; in this second part, we present the optical models representing the two IR channels, SO (Solar Occultation) and LNO (Limb, Nadir and Occultation), and use them to determine signal to noise ratios (SNRs) for many expected observational cases. In solar occultation mode, both the SO and LNO channel exhibit very high SNRs >5000. SNRs of around 100 were found for the LNO channel in nadir mode, depending on the atmospheric conditions, Martian surface properties, and observation geometry., NOMAD has been made possible thanks to funding by the Belgian Science Policy Office (BELSPO) and financial and contractual coordination by the ESA Prodex Office. The research was performed as part of the “Interuniversity Attraction Poles” programme financed by the Belgian government (Planet TOPERS). UK funding is acknowledged under the UK Space Agency grant ST/I003061/1.

Published
2016

44. MAVEN and the total electron content of the Martian ionosphere

Author

Mendillo, Michael, primary, Narvaez, Clara, additional, Vogt, Marissa F., additional, Mayyasi, Majd, additional, Mahaffy, Paul, additional, Benna, Mehdi, additional, Andersson, Laila, additional, Campbell, Bruce, additional, Němec, Frantisek, additional, Ma, Ying Juan, additional, Chaufray, Jean‐Yves, additional, Leblanc, François, additional, Gonzalez‐Galindo, Francisco, additional, Lopez‐Valverde, Miguel Ángel, additional, Forget, François, additional, and Jakosky, Bruce, additional

Published
2017
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45. The Mars Climate Database (MCD version 5.2)

Author

Millour, E., Forget, Francois, Spiga, Aymeric, Navarro, T., Madeleine, Jean-Baptiste, Montabone, Luca, Pottier, Alizée, Lefèvre, Franck, Montmessin, Franck, Chaufray, Jean-Yves, Lopez-Valverde, M. A., Gonzalez-Galindo, Francisco, Lewis, Stephen R., Read, P.L., Huot, Jean-Paul, Desjean, M.-C., Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Space Science Institute [Boulder] (SSI), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), Space Science Institute [Boulder] ( SSI ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), The Open University [Milton Keynes] ( OU ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), European Space Research and Technology Centre ( ESTEC ), European Space Agency ( ESA ), Centre National d'Etudes Spatiales ( CNES ), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Oxford, and Agence Spatiale Européenne = European Space Agency (ESA)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; The Mars Climate Database (MCD) is a database of meteorological fields derived from General Circulation Model (GCM) numerical simulations of the Martian atmosphere and validated using available observational data. The MCD includes complementary post-processing schemes such as high spatial resolution interpolation of environmental data and means of reconstructing the variability thereof. We have just completed (March 2015) the generation of a new version of the MCD, MCD version 5.2.

Published
2015

46. Science objectives and performances of NOMAD, a spectrometer suite for the ExoMars TGO mission

Author

Vandaele, A. C, Neefs, E., Drummond, R., Thomas, I. R., Daerden, F., Lopez Moreno, J. J., Rodriguez, J., Patel, M. R., Bellucci, G., Allen, M., Altieri, F., Bolsée, D., Clancy, T., Delanoye, S., Depiesse, C., Cloutis, E., Fedorova, A., Formisano, V., Funke, B., Fussen, D., Geminale, A., Gérard, J. C., Giuranna, M., Ignatiev, N., Kaminski, J., Karatekin, O., Lefèvre, F., López Puertas, M., López Valverde, M., Mahieux, A., Mcconnell, J., Mumma, M., Neary, L., Renotte, E., Ristic, B., Robert, S., Smith, M., Trokhimovsky, S., Vanderauwera, J., Villanueva, G., Whiteway, J., Wilquet, V., Wolff, M., Vandaele, Ann Carine, Lopez Moreno, Jose Juan, Bellucci, Giancarlo, Patel, Manish, Allen, Mark, Altieri, Francesca, Aoki, Shohei, Bolsée, David, Clancy, Todd, Cloutis, Edward, Daerden, Frank, Depiesse, Cédric, Fedorova, Anna, Formisano, Vittorio, Funke, Bernd, Fussen, Didier, Garcia Comas, Maya, Geminale, Anna, Gérard, Jean Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez Galindo, Francisco, Ignatiev, Nicolai, Kaminski, Jacek, Karatekin, Ozgur, Kasabe, Yasumasa, Lefèvre, Franck, Lewis, Stephen, López Puertas, Manuel, López Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mumma, Mike, Neary, Lori, Neefs, Eddy, Renotte, Etienne, Robert, Séverine, Sindoni, Giuseppe, Smith, Mike, Thomas, Ian R., Trokhimovsky, Sacha, Vander Auwera, Jean, Villanueva, Geronimo, Whiteway, Jim, Willame, Yannick, Wilquet, Valerie, Wolff, Mike, Alonso Rodrigo, Gustavo, Aparicio Del Moral, Beatriz, Barzin, Pascal, Ben Moussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, Sabrina, Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Delanoye, Sofie, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Zafra, Jose Jeronimo, Leese, Mark, Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, Jose, Morales, Rafael, Orban, Anne, Pastor Morales, Maria Del Carmen, Perez Grande, Isabel, Ristic, Bojan, Rodriguez Gomez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan Felipe, Thibert, Tanguy, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), The Open University [Milton Keynes] (OU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, York University [Toronto], Royal Observatory of Belgium [Brussels] (ROB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Centre Spatial de Liège (CSL), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), and Catholic University of America

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Solar, Occultation, law.invention, Orbiter, Mars atmosphere, law, Nadir, Aerosol, Observations, Spectroscopy, Ultraviolet, Remote sensing, Spectrometer, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Suite, Astronomy and Astrophysics, Mars Exploration Program, Atmosphere of Mars, ExoMars, Trace gas, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, Visible, Composition, Infrared, Methane, Occultation Nadir, Environmental science
Abstract

International audience; The NOMAD spectrometer suite on the ExoMars Trace Gas Orbiter will map the composition and distribution of Mars' atmospheric trace species in unprecedented detail, fulfilling many of the scientific objectives of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument is a combination of three channels, covering a spectral range from the UV to the IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and how these objectives have influenced the design of the channels. We also discuss the expected performance of the instrument in terms of coverage and detection sensitivity.

Published
2015
Full Text
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47. Simulating the Mars Climate with the LMD Mars Global Climate Model: validation and issues

Author

Forget , François, Millour , E., Spiga , Aymeric, Madeleine , J.-B., Pottier , Alizée, Navarro , T., Montabone , L., Colaitis , A., Kerber , L., Lefèvre , Franck, Montmessin , Franck, Chaufray , Jean-Yves, Gonzalez-Galindo , Francisco, Lopez-Valverde , M.A., Lewis , S.R., Read , P. L., Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] ( OU ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), University of Oxford [Oxford], F. Forget and M. Millour, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), The Open University [Milton Keynes] (OU), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), Cardon, Catherine, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), and University of Oxford

Subjects
[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], [ PHYS.PHYS.PHYS-AO-PH ] Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.PHYS.PHYS-AO-PH] Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph]
Abstract

International audience; The Mars atmosphere Global Climate Model (GCM) developed at the Laboratoire de Météorologie Dynamique in collaboration with several teams in Europe (LATMOS, University of Oxford, The Open University, the Instituto de Astrofisica de Andalucia), and with the support of ESA and CNES is currently used for many kind of applications. Our primary objective is to predict all details of the Mars Climate system, including the dust, water, CO 2 and photochemical cycles from the surface to the exobase, yet only on the basis of universal equations. In practice, to simulate a given year, we still have to assume a daily map of column dust opacity (See Montabone et al., this issue), but otherwise the model is almost free of other forcing (including to predict the dust vertical distribution). 2013 was an important milestone for the project since it concluded a long series of model development defined on the basis of the analysis of the Mars Climate Database version 4, released in 2005 using a previous version of our GCM (Forget et al. 2006). Key improvements As documented in the previous edition of the Mars Atmosphere Modeling and Observation Workshop, and in the per-review literature:  Improved dynamical core for the polar atmosphere  Improvements of Mars surface fields (albedo and thermal inertia map)  Inclusion of subsurface water ice in the CO 2 ice cap energy balance, and improved tuning of the CO 2 cycle  Improved parametrizations of convection and near surface turbulence, using a thermal plume model This thermal plume model is coupled to surface layer parameterizations taking into account stability and turbulent gustiness to calculate surface-atmosphere fluxes (Colaitis et al. 2013)  Improvement of the representation of the airborne dust (Madeleine et al. 2011) based on a " semi-interactive " two moments dust transport scheme to predict the dust vertical distribution and the 3D variation of dust particle radii, coupled to improved radiative transfer calculations

Published
2014

48. Mars-Solar Wind Interaction: Coupling Between Hybrid, Ionospheric, Thermospheric and Exospheric Models

Author

Leblanc, François, Chaufray, Jean-Yves, Modolo, Ronan, Hess, Sebastien, Yagi, M., Mancini, M., Forget, François, Gonzalez-Galindo, Francisco, Lorenzato, L., Mazelle, Christian, Chanteur, Gérard, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Solar-Terrestrial Environment Laboratory [Nagoya] (STELab), Nagoya University, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des Plasmas (LPP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), HEPPI - LATMOS, ONERA, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-École polytechnique (X)-Sorbonne Universités-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; The solar wind interaction with the Martian neutral envi- ronment is investigated by means of three dimensional hybrid magnetospheric simulations. In such formal- ism, ions have a kinetic description while electrons are treated as an inertialess fluid, ensuring the neutrality of the plasma and contributing to currents and pressure terms. This model has been successfully used to de- scribe the near ionized environment of Mars

Published
2014

49. New nitric oxide (NO) nightglow measurements with SPICAM/MEX as a tracer of Mars upper atmosphere circulation

Author

Bertaux, Jean-Loup, Gagné, Marie-Eve, Montmessin, Franck, Gonzalez-Galindo, Francisco, Lefèvre, Franck, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Toronto], University of Toronto, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and Cardon, Catherine

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

In the upper atmosphere of Mars, CO2 and N2 are photo-dissociated by solar UV and EUV on the day side, producing O and N atoms. They are carried to the night side by planet rotation and general circulation in the thermosphere. When they recombine to form nitric oxide (NO), they emit light in the UV in the so-called δ and γ bands, producing a UV nightglow that was discovered by SPICAM/Mars Express in 2005 during dedicated limb observations. Therefore, it provides an important tracer of thermospheric circulation, tracing mostly descending air. A new data set has been produced by using more frequent star occultations (more than 2000), which in about 10% cases revealed the presence of the NO emission in addition to the star signal. We have developed a method allowing to retrieve the vertical profile of the NO emission intensity, after disentangling the star signal from the limb signal. We have made a first-order comparison with the MGCM LMD model. The peak intensity (a few KiloRayleigh) and the peak altitude (50-100 km) are in reasonable agreement with model predictions. There is a clear seasonal pattern of the latitude location of the emission. The latitude of the emission as a function of season (solar longitude Ls) can be approximated with a relationship of the form Lat= -80 sin (Ls). At solstices (Ls=90 and 270°) this is in agreement with the MGCM model, which predicts an emission in the depth of the winter polar night. At equinoxes (Ls=0 and 180°), the emission is observed near the equator, in total contradiction with the model, which predicts on the contrary an emission simultaneously at both polar regions. The significance of this major discrepancy for the general circulation of the upper atmosphere of Mars will be discussed, and the NO and O2 observed nightglows will be compared.

Published
2013

50. Current status on Mars exospheric studies

Author

Chaufray, Jean-Yves, Leblanc, François, Yagi, Manabu, Bertaux, Jean-Loup, Quémerais, Eric, Modolo, Ronan, Gonzalez-Galindo, Francisco, Lopez-Valverde, Miguel, Forget, François, Clarke, John, Chaffin, Michael, Schneider, Nick, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut Pierre-Simon-Laplace (IPSL), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Boston University [Boston] (BU), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Cardon, Catherine, École normale supérieure - Paris (ENS-PSL), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; The Martian exosphere is the collisionless region surrounding the Martian atmosphere. It is mainly composed of hydrogen and oxygen atoms. The hydrogen and oxygen atoms are produced in the Martian mesosphere-thermosphere from molecular dissociation and reach the exobase by vertical diffusion. A small part of these atoms reaching the exobase can escape into the interplanetary medium leading to a net loss of water. Another part does not escape but populates the exosphere forming an extended corona. In this presentation, we will present results of new models we developed in the frame of the HELIOSARES project to study the Martian exospheric hydrogen and oxygen populations. We will also present a comparison between these results and recent observations of the Martian exosphere done by Mars Express, Hubble Space Telescope and Rosetta.

Published
2012

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