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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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5. 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

10. 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

12. Longitudinal Variations of Mars Thermosphere CO2, Ar, N2, and O Densities From MAVEN: Dependencies on Species Mass, Solar Flux, and Local Time.

Author

Forbes, Jeffrey M., Xiaohua Fang, Xiaoli Zhang, Benna, Mehdi, and González-Galindo, Francisco

Subjects
THERMOSPHERE, ROSSBY waves, STANDING waves, MARTIAN atmosphere, MARS (Planet), ATMOSPHERE
Abstract

Measurements of CO2, Ar, N2, and O densities between 150 and 200 km from the Mars Atmosphere and Volatile Evolution Neutral Gas and Ion Mass Spectrometer during February 2015 to February 2022 are analyzed to provide a comprehensive analysis of their longitudinal wavenumber k = 1, 2, and 3 components. Variations in density amplitudes (Ak) with solar flux are marginally detectable during this period. The Ak binned and averaged in latitude, local solar time and Ls are referenced to diurnal- and zonal-mean backgrounds in accord with how tides and stationary planetary waves (SPWs) are defined in theory and modeling. The resulting global Ak distributions are the interference patterns formed by superposition of diurnal tides, SPWs and/or semidiurnal tides; consequently, a simple dependence on species mass consistent with thermal expansion (diffusive equilibrium) that might exist for some individual wave components is obscured. Additionally, vertical winds likely contribute to deviations from diffusive equilibrium. Complementary analyses of the Mars Climate Database indicate that the major contributors to the Ak are DE2, SE1, DE1, and SPW1, 2, 3; support the absence of significant variability due to solar flux; and indicate a more well-defined sensitivity to species mass. The Ak and their phases (longitudes of maxima) for the whole data set are available as part of Supporting Information S1. [ABSTRACT FROM AUTHOR]

Published
2024
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13. Martian Atmospheric Aerosols Composition and Distribution Retrievals During the First Martian Year of NOMAD/TGO Solar Occultation Measurements: 2. Extended Results, End of MY 34 and First Half of MY 35

Author

Stolzenbach, Aurélien, primary, López Valverde, Miguel‐Angel, additional, Brines, Adrian, additional, Modak, Ashimananda, additional, Funke, Bernd, additional, González‐Galindo, Francisco, additional, Thomas, Ian, additional, Liuzzi, Giuliano, additional, Villanueva, Gerónimo, additional, Luginin, Mikhail, additional, Aoki, Shohei, additional, Grabowski, Udo, additional, Lopez Moreno, José Juan, additional, Rodriguez‐Gomez, Julio, additional, Wolff, Mike, additional, Ristic, Bojan, additional, Daerden, Frank, additional, Bellucci, Giancarlo, additional, Patel, Manish, additional, and Vandaele, Ann‐Carine, additional

Published
2023
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14. Martian Atmospheric Aerosols Composition and Distribution Retrievals During the First Martian Year of NOMAD/TGO Solar Occultation Measurements: 1. Methodology and Application to the MY 34 Global Dust Storm

Author

Stolzenbach, Aurélien, primary, López Valverde, Miguel‐Angel, additional, Brines, Adrian, additional, Modak, Ashimananda, additional, Funke, Bernd, additional, González‐Galindo, Francisco, additional, Thomas, Ian, additional, Liuzzi, Giuliano, additional, Villanueva, Gerónimo, additional, Luginin, Mikhail, additional, Aoki, Shohei, additional, Grabowski, Udo, additional, Lopez Moreno, José Juan, additional, Rodrìguez Gòmez, Julio, additional, Wolff, Mike, additional, Ristic, Bojan, additional, Daerden, Frank, additional, Bellucci, Giancarlo, additional, Patel, Manish, additional, and Vandaele, Ann‐Carine, additional

Published
2023
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16. A Surface to Exosphere Non‐Orographic Gravity Wave Parameterization for the Mars Planetary Climate Model

Author

Liu, Jiandong, primary, Millour, Ehouarn, additional, Forget, François, additional, Gilli, Gabriella, additional, Lott, François, additional, Bardet, Deborah, additional, González Galindo, Francisco, additional, Bierjon, Antoine, additional, Naar, Joseph, additional, Martinez, Antoine, additional, Lebonnois, Sébastien, additional, Fan, Siteng, additional, Pierron, Thomas, additional, and Vandemeulebrouck, Romain, additional

Published
2023
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18. Retrieval of Martian Atmospheric CO Vertical Profiles From NOMAD Observations During the First Year of TGO Operations

Author

Modak, Ashimananda, primary, López‐Valverde, Miguel Angel, additional, Brines, Adrian, additional, Stolzenbach, Aurélien, additional, Funke, Bernd, additional, González‐Galindo, Francisco, additional, Hill, Brittany, additional, Aoki, Shohei, additional, Thomas, Ian, additional, Liuzzi, Giuliano, additional, Villanueva, Gerónimo, additional, Erwin, Justin, additional, Lopez Moreno, José Juan, additional, Yoshida, Nao, additional, Grabowski, Udo, additional, Forget, Francois, additional, Daerden, Frank, additional, Ristic, Bojan, additional, Bellucci, Giancarlo, additional, Patel, Manish, additional, Trompet, Loic, additional, and Vandaele, Ann‐Carine, additional

Published
2023
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20. Martian Atmospheric Temperature and Density Profiles During the First Year of NOMAD/TGO Solar Occultation Measurements

Author

NOMAD Team, López-Valverde, Miguel Angel, Funke, Bernd, Brines, Adrian, Stolzenbach, Aurèlien, Modak, Ashimananda, Hill, Brittany, González-Galindo, Francisco, Thomas, Ian, Trompet, Loic, Aoki, Shohei, Villanueva, Gerónimo, Liuzzi, Giuliano, Erwin, Justin, Grabowski, Udo, Forget, Francois, López-Moreno, José Juan, Rodriguez-Gómez, Julio, Ristic, Bojan, Daerden, Frank, Bellucci, Giancarlo, Patel, Manish, Vandaele, Ann-Carine, Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, and UK Space Agency

Subjects
Atmosphere, IAA, KOPRA, Temperature, Mars, Density, ExoMars/TGO, Earth sciences, RCP, Geophysics, IMK-ASF-SAT, Remote sounding, Atmospheric structure, Space and Planetary Science, Geochemistry and Petrology, ddc:550, TGO, Earth and Planetary Sciences (miscellaneous), NOMAD, Planetary atmospheres
Abstract

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We present vertical profiles of temperature and density from solar occultation (SO) observations by the “Nadir and Occultation for Mars Discovery” (NOMAD) spectrometer on board the Trace Gas Orbiter during its first operational year, which covered the second half of Mars Year 34. We used calibrated transmittance spectra in 380 scans, and apply an in-house pre-processing to clean data systematics. Temperature and CO2 profiles up to about 90 km, with consistent hydrostatic adjustment, are obtained, after adapting an Earth-tested retrieval scheme to Mars conditions. Both pre-processing and retrieval are discussed to illustrate their performance and robustness. Our results reveal the large impact of the MY34 Global Dust Storm (GDS), which warmed the atmosphere at all altitudes. The large GDS aerosols opacity limited the sounding of tropospheric layers. The retrieved temperatures agree well with global climate models (GCM) at tropospheric altitudes, but NOMAD mesospheric temperatures are wavier and globally colder by 10 K in the perihelion season, particularly during the GDS and its decay phase. We observe a warm layer around 80 km during the Southern Spring, especially in the Northern Hemisphere morning terminator, associated to large thermal tides, significantly stronger than in the GCM. Cold mesospheric pockets, close to CO2 condensation temperatures, are more frequently observed than in the GCM. NOMAD CO2 densities show oscillations upon a seasonal trend that track well the latitudinal variations expected. Results uncertainties and suggestions to improve future data re-analysis are briefly discussed. © 2022 The Authors. This article has been contributed to by U.S. Government employees and their work is in the public domain in the USA., The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCI through the ‘Center of Excellence Severe Ochoa’ award for the Instituto de Astrofísica de Andalucia (DEV-2017-0709) and funding by grants PGC2018-101836-B-100 (MCI/AEI/FEDER, EU), PID2019-110689RB-I00/AEI/10.13039/501100011033, and RTI2018-100920-J-I00. ExoMars is a space mission of the European Space Agency (ESA) and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELLS), with the financial and contractual coordination by the ESAU Prod ex Office (PEA 4000103401, 4000121493) as well as by UK Space Agency through Grant ST/V002295/1, ST/V005332/1 and ST/S00145X/1 and Italian Space Agency through Grant 2018-2-HHS.0. US investigators were supported by the National Aeronautics and Space Administration. This work was supported by the Belgian Funds de la Recherche Scientific—FIRS under Grant 30442502 (ET_HOME). This project has received funding from the European Union Horizon 2020 research and innovation program under grant agreement No 101004052 (Road Map project)., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).

Published
2023

23. Simulation of the Hydrogen escape from Mars using a Global Climate Model

Author

González-Galindo, Francisco, primary, Chaufray, Jean-Yves, additional, Gilli, Gabriella, additional, Vals, Margaux, additional, Lefèvre, Franck, additional, Montmessin, Franck, additional, Rossi, Loic, additional, Forget, Francois, additional, Millour, Ehouarn, additional, López-Valverde, Miguel Ángel, additional, and Brines, Adrián, additional

Published
2022
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24. Characterization of the Martian mesosphere with NOMAD/TGO observations and a Global Climate Model

Author

González-Galindo, Francisco, primary, López-Valverde, Miguel Ángel, additional, Brines, Adrián, additional, Modak, Ashimananda, additional, Stolzenbach, Aurélien, additional, Funke, Bernd, additional, López-Moreno, José Juan, additional, Forget, Francois, additional, Millour, Ehouarn, additional, Lefèvre, Franck, additional, Vals, Margaux, additional, Montmessin, Franck, additional, Patel, Manish, additional, Bellucci, Giancarlo, additional, and Vandaele, Ann-Carine, additional

Published
2022
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25. Global troposphere-to-msosphre modelling of martian CO2 ice clouds

Author

Määttänen, Anni, primary, Mathé, Christophe, additional, Audouard, Joachim, additional, Listowski, Constantino, additional, Millour, Ehouarn, additional, Forget, Francois, additional, González-Galindo, Francisco, additional, Falletti, Lola, additional, Bardet, Deborah, additional, Teinturier, Lucas, additional, Vals, Margaux, additional, Spiga, Aymeric, additional, and Montmessin, Franck, additional

Published
2022
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26. Differential Ablation of meteoric metals in the LMD-Mars-Metals and NCAR WACCM-Metals models

Author

Feng, Wuhu, primary, Plane, John, additional, González-Galindo, Francisco, additional, Marsh, Daniel, additional, Chipperfield, Martyn, additional, Carrillo-Sánchez, Juan Diego, additional, Janches, Diego, additional, Chaufray, Jean-Yves, additional, Forget, Francois, additional, Millour, Ehouarn, additional, Crismani, Matteo, additional, Tyo, Robert, additional, Schneider, Nicholas, additional, and Benna, Mehdi, additional

Published
2022
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27. Composition and size of Martian aerosols as seen in the IR from solar occultation measurements by NOMAD onboard TGO

Author

stolzenbach, aurélien, primary, López Valverde, Miguel-Angel, additional, Brines, Adrian, additional, Modak, Ashimananda, additional, Funke, Bernd, additional, González-Galindo, Francisco, additional, Thomas, Ian, additional, Liuzzi, Giuliano, additional, Villanueva, Geronimo, additional, Luginin, Mikhail, additional, and Aoki, Shohei, additional

Published
2022
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28. Solar‐Synchronous Tides in Mars Thermosphere CO2, Ar, and N2 Densities From MAVEN.

Author

Forbes, Jeffrey M., Zhang, Xiaoli, Fang, Xiaohua, Benna, Mehdi, González‐Galindo, Francisco, Forget, Francois, and Millour, Ehouarn

Subjects
MARTIAN atmosphere, MARS (Planet), THERMOSPHERE, SOLAR oscillations, THERMAL expansion, MASS spectrometers
Abstract

Measurements of CO2, Ar and N2 densities from the Neutral Gas and Ion Mass Spectrometer on the Mars Atmosphere and Volatile Evolution Mission (MAVEN) between 150 and 200 km altitude during 2015–2022 are analyzed to reveal diurnal (DW1), semidiurnal (SW2) and terdiurnal (TW3) solar‐synchronous tides in Mars thermosphere. Multi‐year‐mean tidal perturbations on a diurnal‐ and zonal‐mean background, corrected for solar flux variations, are reported as a function of latitude (48°S–48°N), altitude and solar longitude (Ls). The DW1, SW2 and TW3 amplitudes at for example, 180 km altitude are of order 90%–120%, 15%–20%, and ≲10% for CO2 and Ar, and roughly 2/3 these values for N2, the latter presumably due to the difference in molecular weight from the other species. Through examination of vertical phase progressions, DW1 is concluded to be mainly excited in situ, but SW2 and TW3 contain significant contributions from tides propagating upward from lower altitudes. By analogy with studies for Earth's thermosphere, the DW1 amplitudes and phases are thought to reflect the combined influences of thermal expansion and vertical winds. Points of agreement and disagreement with DW1, SW2, and TW3 amplitudes and phases derived from the Mars Climate Database are noted and interpreted. Key Points: Global‐scale solar‐synchronous tides are derived from Mars Atmosphere and Volatile Evolution Mission/Neutral Gas and Ion Mass Spectrometer measurements of CO2, Ar, and N2 at Mars, 150–200 kmThe diurnal tide originates mainly in situ; semidiurnal and terdiurnal tides show evidence of upward propagation from belowPoints of agreement and disagreement with the Mars Climate Database are noted and interpreted [ABSTRACT FROM AUTHOR]

Published
2023
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29. Investigations of the Mars Upper Atmosphere with ExoMars Trace Gas Orbiter

Author

López-Valverde, Miguel A., Gerard, Jean-Claude, González-Galindo, Francisco, Vandaele, Ann-Carine, Thomas, Ian, Korablev, Oleg, Ignatiev, Nikolai, Fedorova, Anna, Montmessin, Franck, Määttänen, Anni, Guilbon, Sabrina, Lefevre, Franck, Patel, Manish R., Jiménez-Monferrer, Sergio, García-Comas, Maya, Cardesin, Alejandro, Wilson, Colin F., Clancy, R. T., Kleinböhl, Armin, McCleese, Daniel J., Kass, David M., Schneider, Nick M., Chaffin, Michael S., López-Moreno, José Juan, and Rodríguez, Julio

Published
2018
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30. Mars Express science highlights and future plans

Author

Titov, Dmitrij, primary, Wilson, Colin, additional, Bibring, Jean-Pierre, additional, Cardesin, Alejandro, additional, Carter, John, additional, Duxbury, Tom, additional, Forget, Francois, additional, Giuranna, Marco, additional, González-Galindo, Francisco, additional, Holmström, Mats, additional, Jaumann, Ralf, additional, Määttänen, Anni, additional, Martin, Patrick, additional, Montmessin, Franck, additional, Orosei, Roberto, additional, Pätzold, Martin, additional, Plaut, Jeff, additional, and Sgs Team, Mex, additional

Published
2022
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31. Martian Atmospheric Temperature and Density Profiles During the First Year of NOMAD/TGO Solar Occultation Measurements.

Author

López‐Valverde, Miguel Angel, Funke, Bernd, Brines, Adrian, Stolzenbach, Aurèlien, Modak, Ashimananda, Hill, Brittany, González‐Galindo, Francisco, Thomas, Ian, Trompet, Loic, Aoki, Shohei, Villanueva, Gerónimo, Liuzzi, Giuliano, Erwin, Justin, Grabowski, Udo, Forget, Francois, López‐Moreno, José Juan, Rodriguez‐Gómez, Julio, Ristic, Bojan, Daerden, Frank, and Bellucci, Giancarlo

Subjects
ATMOSPHERIC temperature, ATMOSPHERIC density, CLIMATE change models, FRONTS (Meteorology), DUST storms, GLOBAL warming
Abstract

We present vertical profiles of temperature and density from solar occultation (SO) observations by the "Nadir and Occultation for Mars Discovery" (NOMAD) spectrometer on board the Trace Gas Orbiter during its first operational year, which covered the second half of Mars Year 34. We used calibrated transmittance spectra in 380 scans, and apply an in‐house pre‐processing to clean data systematics. Temperature and CO2 profiles up to about 90 km, with consistent hydrostatic adjustment, are obtained, after adapting an Earth‐tested retrieval scheme to Mars conditions. Both pre‐processing and retrieval are discussed to illustrate their performance and robustness. Our results reveal the large impact of the MY34 Global Dust Storm (GDS), which warmed the atmosphere at all altitudes. The large GDS aerosols opacity limited the sounding of tropospheric layers. The retrieved temperatures agree well with global climate models (GCM) at tropospheric altitudes, but NOMAD mesospheric temperatures are wavier and globally colder by 10 K in the perihelion season, particularly during the GDS and its decay phase. We observe a warm layer around 80 km during the Southern Spring, especially in the Northern Hemisphere morning terminator, associated to large thermal tides, significantly stronger than in the GCM. Cold mesospheric pockets, close to CO2 condensation temperatures, are more frequently observed than in the GCM. NOMAD CO2 densities show oscillations upon a seasonal trend that track well the latitudinal variations expected. Results uncertainties and suggestions to improve future data re‐analysis are briefly discussed. Plain Language Summary: The detailed variation of temperature and density with altitude is of paramount importance to characterize the atmospheric state and to constrain the chemistry and dynamics as a whole. The Nadir and Occultation for Mars Discovery (NOMAD) instrument on board the Trace Gas Orbiter (TGO) has among its key targets the characterization of the thermal state with unprecedented vertical resolution. This is the target of this work, where we analyzed transmittance spectra obtained from the NOMAD solar occultation channel, with a state‐of‐the‐art retrieval scheme, adapted from Earth to Mars conditions and geometry. We applied it to the first year of TGO observations, which covered the last two Mars seasons of Mars Year 34. The results permit to study the temperature structure up to 90 km and its seasonal and latitudinal variations, revealing the impact of the MY34 Global Dust Storm, a warm layer at mesospheric altitudes not present in climate models, more frequent cold pockets than in current global climate models, and generally, colder temperature at those altitudes, all of which can be of importance for the validation of these climate models. Key Points: Temperature and density profiles up to 90 km are retrieved from Nadir and Occultation for Mars Discovery (NOMAD) first year of solar occultations, covering two seasons of Mars Year 34NOMAD temperatures agree well with climate model predictions below 50 km but are wavier and globally colder by about 10 K at high altitudesWe report large thermal tides producing warm layers at 80 km in the morning terminator. Also strong warming by the 2018 global dust storm [ABSTRACT FROM AUTHOR]

Published
2023
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32. A global model of meteoric metals in the atmosphere of Mars

Author

Feng, Wuhu, primary, Plane, John, additional, González-Galindo, Francisco, additional, Marsh, Daniel, additional, Welch, Adam, additional, Carrillo-Sánchez, Juan Diego, additional, Janches, Diego, additional, Chaufray, Jean-Yves, additional, Forget, Francois, additional, Millour, Ehouarn, additional, Crismani, Matteo, additional, Schneider, Nicholas, additional, and Benna, Mehdi, additional

Published
2021
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33. Martian water vapor vertical profiles from solar occultation measurements by NOMAD onboard TGO/ExoMars: H2O-Temperature retrievals with the IAA-KOPRA forward model

Author

Brines, Adrian, primary, Lopez-Valverde, Miguel Angel, additional, Stolzenbach, Aurélien, additional, Modak, Ashimananda, additional, Hill, Brittany, additional, Funke, Bernd, additional, González-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, additional, Liuzzi, Giuliano, additional, Patel, Manish, additional, and Bellucci, Giancarlo, additional

Published
2021
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36. Mars Express science highlights and future plans

Author

Titov, Dmitrij, primary, Bibring, Jean-Pierre, additional, Cardesin, Alejandro, additional, Carter, John, additional, Duxbury, Tom, additional, Forget, Francois, additional, Giuranna, Marco, additional, González-Galindo, Francisco, additional, Holmström, Mats, additional, Jaumann, Ralf, additional, Määttänen, Anni, additional, Martin, Patrick, additional, Montmessin, Franck, additional, Orosei, Roberto, additional, Pätzold, Martin, additional, Plaut, Jeffrey, additional, and Sgs Team, Mex, additional

Published
2021
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37. CO2 and Temperature vertical profiles in the Martian atmosphere from solar occultation measurements  at 2.7 micron by instruments NOMAD and ACS  on board the Exomars Trace Gas Orbiter 

Author

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

Published
2021
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44. The Mars Climate Database (MCD version 5.3)

Author

Millour, Ehouarn, Forget, Francois, Spiga, Aymeric, Vals, Margaux, Zakharov, Vladimir, Montabone, Luca, Lefèvre, Franck, Montmessin, Franck, Chaufray, Jean-Yves, López-Valverde, Miguel, González-Galindo, Francisco, Lewis, Stephen, Read, Peter, Desjean, Marie-Christine, and Cipriani, Fabrice

Abstract

21st EGU General Assembly, EGU2019, Proceedings from the conference held 7-12 April, 2019 in Vienna, Austria, id.7153, Our Global Circulation Model (GCM) simulates the atmospheric environment of Mars. It is developped at LMD (Laboratoire de Meteorologie Dynamique, Paris, France) in close collaboration with several teams in Europe (LATMOS, France, University of Oxford, The Open University, the Instituto de Astrofisica de Andalucia), and with the support of ESA (European Space Agency) and CNES (French Space Agency). GCM outputs are compiled to build a Mars Climate Database, a freely available tool useful for the scientific and engineering communities. The Mars Climate Database (MCD) has over the years been distributed to more than 350 teams around the world. The latest series of reference simulations have been compiled in version 5.3 of the MCD which was released in 2017. To summarize, MCD v5.3 provides: - Climatologies over a series of synthetic dust scenarios: standard (climatology) year, cold (ie: low dust), warm (ie: dusty atmosphere) and dust storm, all topped by various cases of Extreme UV solar inputs (low, mean or maximum). These scenarios have been derived from home-made, instrument-derived (TES, THEMIS, MCS, MERs), dust climatology of the last 8 Martian years. The MCD also provides simulation outputs (MY24-33) representative of these actual years. - Mean values and statistics of main meteorological variables (atmospheric temperature, density, pressure and winds), as well as surface pressure and temperature, CO2 ice cover, thermal and solar radiative fluxes, dust column opacity and mixing ratio, [H20] vapor and ice columns, concentrations of many species: [CO], [O2], [O], [N2], [H2], [O3], ... - A high resolution mode which combines high resolution (32 pixel/degree) MOLA topography records and Viking Lander 1 pressure records with raw lower resolution GCM results to yield, within the restriction of the procedure, high resolution values of atmospheric variables. - The possibility to reconstruct realistic conditions by combining the provided climatology with additional large scale and small scale perturbations schemes. At EGU, we will report on the latest improvements in the Mars Climate Database, with comparisons with available measurements from orbit (e.g.: TES, MCS, TGO) and landers (Viking, Phoenix, Curiosity).

Published
2019

45. Spatial, Seasonal, and Solar Cycle Variations of the Martian Total Electron Content (TEC): Is the TEC a Good Tracer for Atmospheric Cycles?

Author

Sánchez‐Cano, Beatriz, primary, Lester, Mark, additional, Witasse, Olivier, additional, Blelly, Pierre‐Louis, additional, Indurain, Mikel, additional, Cartacci, Marco, additional, González‐Galindo, Francisco, additional, Vicente‐Retortillo, Álvaro, additional, Cicchetti, Andrea, additional, and Noschese, Raffaella, additional

Published
2018
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46. Mars-solar wind interaction: LatHyS, an improved parallel 3-D multispecies hybrid model

Author

Modolo, Ronan, Hess, Sebastien, Mancini, Marco, Leblanc, François, Chaufray, Jean-Yves, Brain, David, Leclercq, Ludivine, Esteban Hernandez, Rosa, Chanteur, Gérard, Weill, Philippe, González-Galindo, Francisco, Forget, François, Yagi, Manabu, Mazelle, Christian, 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 [Toulouse], ONERA, 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), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], 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), 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), 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), Tohoku University [Sendai], 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), Agence Nationale de la Recherche (ANR), Centre National d'Etudes Spatiales (CNES), International Space Science Institute (ISSI), European Commission, ANR-09-BLAN-0223,HELIOSARES,Relation Soleil ? Mars: description et analyse des échanges présents et passés entre magnétosphère et atmosphère(2009), European Project: 262863,EC:FP7:SPA,FP7-SPACE-2010-1,IMPEX(2011), 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), 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), 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), Université Toulouse III - Paul Sabatier (UT3), 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), 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), HEPPI - LATMOS, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Physics::Space Physics, magnetosphere, interaction, Mars, plasma, Simulation
Abstract

International audience In order to better represent Mars-Solar wind interaction, we present an unprecedented model achieving spatial resolution down to 50 km, a so far unexplored resolution for global kinetic models of the Martian ionized environment. Such resolution approaches the ionospheric plasma scale height. In practice, the model is derived from a first version described in Modolo et al. [2005]. An important effort of parallelization has been conducted and is presented here. A better description of the ionosphere was also implemented including ionospheric chemistry, electrical conductivities and a drag force modelling the ion-neutral collisions in the ionosphere. This new version of the code, named LatHyS (Latmos Hybrid Simulation), is here used to characterize the impact of various spatial resolutions on simulation results. In addition, and following a global model challenge effort [Brain et al., 2010], we present the results of simulation run for three cases which allows addressing the effect of the supra-thermal corona and of the solar EUV activity on the magnetospheric plasma boundaries and on the global escape. Simulation results showed that global patterns are relatively similar for the different spatial resolution runs but finest grid runs provide a better representation of the ionosphere and display more details of the planetary plasma dynamic. Simulation results suggest that a significant fraction of escaping O+ ions is originated from below 1200 km altitude.

Published
2016

48. The Martian ionosphere: comparison of a global climate model with MARSIS data

Author

González-Galindo, Francisco, Nemec, F., Lopez-Valverde, Miguel, Chaufray, Jean-Yves, Forget, Francois, Morgan, D.D., Diéval, C., Gurnett, D. A., Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague] (CU), 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), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], 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 Cardon, Catherine

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; We present here the comparison of the electron den- sity profiles predicted by a 3D global climate model (GCM), the Mars GCM developed at the Laboratoire de Météorologie Dynamique (LMD-MGCM) [4], with the measurements from the instrument MARSIS on board Mars Express [5]. The observations were ob- tained during 5 Martian Years (MY), from MY27 to MY31 (mid 2005-end of 2013). The model was run using the observed day-to-day variability of the UV solar flux and of the dust load during that period. We focus the comparison on two parameters: the electron density at the main peak, and the altitude of the peak. Special attention will be paid to the variability of these two parameters with different geophysical parameters (latitude, SZA, ...), which can provide interesting in- formation about the neutral upper atmosphere of Mars and its interaction with the UV solar radiation.

Published
2015

49. Global distributions of CO2 volume mixing ratio in the middle and upper atmosphere from daytime MIPAS high-resolution spectra

Author

Jurado-Navarro, Á. Aythami, primary, López-Puertas, Manuel, additional, Funke, Bernd, additional, García-Comas, Maya, additional, Gardini, Angela, additional, González-Galindo, Francisco, additional, Stiller, Gabriele P., additional, Clarmann, Thomas von, additional, Grabowski, Udo, additional, and Linden, Andrea, additional

Published
2016
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