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1. Thermal Tides in the Martian Atmosphere near Northern Summer Solstice Observed by ACS/TIRVIM onboard TGO

Author

Fan, Siteng, Guerlet, Sandrine, Forget, François, Bierjon, Antoine, Millour, Ehouarn, Ignatiev, Nikolay, Shakun, Alexey, Grigoriev, Alexey, Trokhimovskiy, Alexander, Montmessin, Franck, and Korablev, Oleg

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Thermal tides in the Martian atmosphere are analyzed using temperature profiles retrieved from nadir observations obtained by the TIRVIM Fourier-spectrometer, part of the Atmospheric Chemistry Suite (ACS) onboard the ExoMars Trace Gas Orbiter (TGO). The data is selected near the northern summer solstice at solar longitude (LS) 75{\deg}-105{\deg} of Martian Year (MY) 35. The observations have a full local time coverage, which enables analyses of daily temperature anomalies. The observed zonal mean temperature is lower by 4-6K at ~100Pa, but higher towards the summer pole, compared to the LMD Mars General Circulation Model (GCM). Wave mode decomposition shows dominant diurnal tide and important semi-diurnal tide and diurnal Kelvin wave, with maximal amplitudes of 5K, 3K, and 2.5K, respectively, from tens to hundreds of Pa. The results generally agree well with the LMD Mars GCM, but with noticeable earlier phases of diurnal (~1h) and semi-diurnal (~3h) tides., Comment: 7 pages, 4 figures, accepted by GRL

Published
2022
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3. First detection of ozone in the mid-infrared at Mars: implications for methane detection

Author

Olsen, Kevin S., Lefèvre, Franck, Montmessin, Franck, Trokhimovskiy, Alexander, Baggio, Lucio, Fedorova, Anna, Alday, Juan, Lomakin, Alexander, Belyaev, Denis A., Patrakeev, Andrey, Shakun, Alexey, and Korablev, Oleg

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract

The ExoMars Trace Gas Orbiter (TGO) was sent to Mars in March 2016 to search for trace gases diagnostic of active geological or biogenic processes. We report the first observation of the spectral features of Martian ozone (O3) in the mid-infrared range using the Atmospheric Chemistry Suite (ACS) Mid-InfaRed (MIR) channel, a cross-dispersion spectrometer operating in solar occultation mode with the finest spectral resolution of any remote sensing mission to Mars. Observations of ozone were made at high northern latitudes (>65N) prior to the onset of the 2018 global dust storm (Ls = 163-193). During this fast transition phase between summer and winter ozone distribution, the O3 volume mixing ratio observed is 100-200 ppbv near 20 km. These amounts are consistent with past observations made at the edge of the southern polar vortex in the ultraviolet range. The observed spectral signature of ozone at 3000-3060 cm-1 directly overlaps with the spectral range of the methane (CH4) nu3 vibration-rotation band, and it, along with a newly discovered CO2 band in the same region, may interfere with measurements of methane abundance., Comment: 7 pages, 6 figures

Published
2020
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4. Martian water ice clouds during the 2018 global dust storm as observed by the ACS-MIR channel onboard the Trace Gas Orbiter

Author

Stcherbinine, Aurélien, Vincendon, Mathieu, Montmessin, Franck, Wolff, Michael, Korablev, Oleg, Fedorova, Anna, Trokhimovskiy, Alexander, Patrakeev, Andrey, Lacombe, Gaëtan, Baggio, Lucio, and Shakun, Alexey

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The Atmospheric Chemistry Suite (ACS) instrument onboard the ExoMars Trace Gas Orbiter (TGO) ESA-Roscosmos mission began science operations in March 2018. ACS Mid InfraRed (MIR) channel notably provides solar occultation observations of the martian atmosphere in the 2.3 - 4.2 $\mu$m spectral range. Here we use these observations to characterize water ice clouds before and during the MY 34 Global Dust Storm (GDS). We developed a method to detect water ice clouds with mean particle size $\leq$ 2 $\mu$m, and applied it to observations gathered between $L_s=165^\circ$ and $L_s=243^\circ$. We observe a shift in water ice clouds maximum altitudes from about 60 km before the GDS to above 90 km during the storm. These very high altitude, small-sized ($r_\mathrm{eff} \leq 0.3$ $\mu$m) water ice clouds are more frequent during MY34 compared to non-GDS years at the same season. Particle size frequently decreases with altitude, both locally within a given profile and globally in the whole dataset. We observe that the maximum altitude at which a given size is observed can increase during the GDS by several tens of km for certain sizes. We notably notice some large water ice particles ($r_\mathrm{eff}\geq1.5$ $\mu$m) at surprisingly high altitudes during the GDS (50 - 70 km). These results suggest that GDS can significantly impact the formation and properties of high altitude water ice clouds as compared to the usual perihelion dust activity.

Published
2019
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6. Untitled Document

Author

Olsen, Kevin S., primary, Fedorova, Anna A., additional, Kass, David M., additional, Kleinböhl, Armin, additional, Trokhimovskiy, Alexander, additional, Korablev, Oleg I, additional, Montmessin, Franck, additional, Lefèvre, Franck, additional, Baggio, Lucio, additional, Alday, Juan, additional, Belyaev, Denis A., additional, Holmes, James A., additional, Mason, Jonathon P., additional, Streeter, Paul M., additional, Rajendran, Kylash, additional, Patel, Manish R, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2024
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8. The chlorine cycle on Mars: What do we know after three Mars years of observation with ACS on TGO?

Author

Olsen, Kevin S., primary, Trokhimovskiy, Alexander, additional, Fedorova, Anna A., additional, Kleinbohl, Armin, additional, Lefèvre, Franck, additional, Montmessin, Franck, additional, Korablev, Oleg I., additional, Alday, Juan, additional, Baggio, Lucio, additional, Belyaev, Denis A., additional, Patrakeev, Andrey S., additional, Shakun, Alexey, additional, and Patel, Manish, additional

Published
2023
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10. Photochemistry on Mars reduces the abundance of heavy isotopes in atmospheric CO and their escape efficiency to space

Author

Alday, Juan, primary, Trokhimovskiy, Alexander, additional, Patel, Manish, additional, Fedorova, Anna, additional, Lefèvre, Franck, additional, Montmessin, Franck, additional, Holmes, James, additional, Rajendran, Kylash, additional, Mason, Jon, additional, Olsen, Kevin, additional, Belyaev, Denis, additional, Korablev, Oleg, additional, Baggio, Lucio, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2023
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11. A Two‐Martian Years Survey of the Water Vapor Saturation State on Mars Based on ACS NIR/TGO Occultations

Author

Fedorova, Anna, primary, Montmessin, Franck, additional, Trokhimovskiy, Alexander, additional, Luginin, Mikhail, additional, Korablev, Oleg, additional, Alday, Juan, additional, Belyaev, Denis, additional, Holmes, James, additional, Lefevre, Franck, additional, Olsen, Kevin, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2022
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14. 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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15. Upper limits on volcanic gases in the Martian atmosphere from the ACS MIR instrument

Author

Braude, Ashwin, primary, Montmessin, Franck, additional, Olsen, Kevin, additional, Trokhimovskiy, Alexander, additional, Korablev, Oleg, additional, Lefèvre, Franck, additional, Fedorova, Anna, additional, Alday, Juan, additional, Baggio, Lucio, additional, Irbah, Abdanour, additional, Lacombe, Gaetan, additional, Forget, François, additional, Millour, Ehouarn, additional, Wilson, Colin, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2022
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16. Measurements of HDO and the D/H ratio in the Martian atmosphere from ACS MIR

Author

Braude, Ashwin, primary, Montmessin, Franck, additional, Olsen, Kevin, additional, Vals, Margaux, additional, Alday, Juan, additional, Rossi, Loïc, additional, Trokhimovskiy, Alexander, additional, Fedorova, Anna, additional, Schmidt, Frédéric, additional, Korablev, Oleg, additional, Lefèvre, Franck, additional, Baggio, Lucio, additional, Irbah, Abdanour, additional, Lacombe, Gaetan, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2022
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17. A Four-Year Search of Methane on Mars with ACS onboard ExoMars TGO

Author

Montmessin, Franck, primary, Korablev, Oleg, additional, Trokhimovskiy, Alexander, additional, Olsen, Kevin, additional, Lefèvre, Franck, additional, Baggio, Lucio, additional, Braude, Ashwin, additional, Fedorova, Anna, additional, Knutsen, Elise, additional, Irbah, Abdanour, additional, Lacombe, Gaétan, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2022
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18. Climatology of the CO Vertical Distribution on Mars Based on ACS TGO Measurements

Author

Fedorova, Anna, primary, Trokhimovskiy, Alexander, additional, Lefèvre, Franck, additional, Olsen, Kevin S., additional, Korablev, Oleg, additional, Montmessin, Franck, additional, Ignatiev, Nikolay, additional, Lomakin, Alexander, additional, Forget, Francois, additional, Belyaev, Denis, additional, Alday, Juan, additional, Luginin, Mikhail, additional, Smith, Michael, additional, Patrakeev, Andrey, additional, Shakun, Alexey, additional, and Grigoriev, Alexey, additional

Published
2022
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19. Assimilation of Temperatures and Column Dust Opacities Measured by ExoMars TGO‐ACS‐TIRVIM During the MY34 Global Dust Storm

Author

Young, Roland M. B., primary, Millour, Ehouarn, additional, Guerlet, Sandrine, additional, Forget, François, additional, Ignatiev, Nikolay, additional, Grigoriev, Alexey V., additional, Shakun, Alexey V., additional, Trokhimovskiy, Alexander, additional, Montmessin, Franck, additional, and Korablev, Oleg, additional

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

Author

Ministerio de Ciencia e Innovación (España), European Commission, Vals, Margaux, Rossi, Loïc., Montmessin, Franck, Lefèvre, Franck, González-Galindo, F., Fedorova, Anna, Luginin, Mikhail, Forget, François, Millour, Ehouarn, Korablev, Oleg, Trokhimovskiy, Alexander, Shakun, Alexey, Bierjon, Antoine, Montabone, Luca, Ministerio de Ciencia e Innovación (España), European Commission, Vals, Margaux, Rossi, Loïc., Montmessin, Franck, Lefèvre, Franck, González-Galindo, F., Fedorova, Anna, Luginin, Mikhail, Forget, François, Millour, Ehouarn, Korablev, Oleg, Trokhimovskiy, Alexander, Shakun, Alexey, Bierjon, Antoine, and Montabone, Luca

Abstract

HDO and the D/H ratio are essential to understand Mars past and present climate, in particular with regard to the evolution through ages of the Martian water cycle. We present here new modeling developments of the HDO cycle with the Laboratoire de Météorologie Dynamique Mars Global Climate Model (GCM). The present study aims at exploring the behavior of the D/H ratio cycle and its sensitivity to the modeling of water ice clouds and the formulation of the fractionation by condensation. Our GCM simulations are compared with observations provided by the Atmospheric Chemistry Suite (ACS) on board the ESA/Roscosmos Trace Gas Orbiter (TGO), and reveal that the model quite well reproduces the temperature and water vapor fields, which offers a good basis for representing the D/H ratio cycle. The comparison also emphasizes the importance of modeling the state of supersaturation, resulting from the microphysical processes of water ice clouds, to correctly account for the water vapor and the D/H ratio of the middle-to-upper atmosphere. This work comes jointly with a detailed comparison of the measured D/H profiles by TGO/ACS and the model outputs, conducted in the companion paper of Rossi et al. (2022, https://doi.org/10.1029/2022JE007201) (this issue). © 2022. The Authors.

Published
2022

22. Publisher Correction: No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations

Author

Korablev, Oleg, Vandaele, Ann Carine, Montmessin, Franck, Fedorova, Anna A., Trokhimovskiy, Alexander, Forget, François, Lefèvre, Franck, Daerden, Frank, Thomas, Ian R., Trompet, Loïc, Erwin, Justin T., Aoki, Shohei, Robert, Séverine, Neary, Lori, Viscardy, Sébastien, Grigoriev, Alexey V., Ignatiev, Nikolay I., Shakun, Alexey, Patrakeev, Andrey, Belyaev, Denis A., Bertaux, Jean-Loup, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Ivanov, Yuriy S., Ristic, Bojan, Mason, Jon, Willame, Yannick, Depiesse, Cédric, Hetey, Laszlo, Berkenbosch, Sophie, Clairquin, Roland, Queirolo, Claudio, Beeckman, Bram, Neefs, Eddy, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, Jose-Juan, Wilson, Colin F., Etiope, Giuseppe, Zelenyi, Lev, Svedhem, Håkan, Vago, Jorge L., and The ACS and NOMAD Science Teams

Published
2019
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23. 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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25. A two-Martian year survey of the water vapor saturation state on Mars based on ACS NIR/TGO occultations

Author

Fedorova, Anna A., primary, Montmessin, Franck, additional, Trokhimovskiy, Alexander, additional, Luginin, Mikhail, additional, Korablev, Oleg I, additional, Alday, Juan, additional, Belyaev, Denis A., additional, Holmes, James Andrew, additional, Lefèvre, Franck, additional, Olsen, Kevin Sutherland, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2022
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27. Seasonal changes in the vertical structure of ozone in the Martian lower atmosphere and its relationship to water vapour

Author

Olsen, Kevin, primary, Fedorova, Anna, additional, Trokhimovskiy, Alexander, additional, Montmessin, Franck, additional, Lefèvre, Franck, additional, Korablev, Oleg, additional, Baggio, Lucio, additional, Forget, Francois, additional, Millour, Ehouarn, additional, Bierjon, Antoine, additional, Alday, Juan, additional, Wilson, Colin, additional, Irwin, Patrick, additional, Belyaev, Denis, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2022
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28. Upper atmosphere as seen by Atmospheric Chemistry Suite onboard ExoMars Trace Gas Orbiter

Author

Korablev, Oleg, Belyaev, Denis, Fedorova, Anna, Trokhimovskiy, Alexander, Montmessin, Franck, Shakun, Alexey, Alday, Juan, Starichenko, Ekaterina, and Cardon, Catherine

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

The ACS instrument onboard the ExoMars TGO dedicated atmospheric spacecraft has been successfully operating since March 2018, delivering unique new data. The processes of water dissipation and the boundary where the lower atmosphere interacts with the exosphere were explored. We will report a selection of results obtained from ACS solar occultations, emphasising the upper part of profiles probing the limits of the neutral atmosphere. The atmospheric profiles were obtained from the strongest CO2 bands up to 200 km altitude. The homopause altitude variation with season was studied. Gravity waves were detected and quantified. Also, the vertical distribution of atmospheric water vapour was measured up to 120 km, resulting in, combined with the altitude profiles of hydrogen and oxygen isotope ratios in CO2 and H2O, implications on the escape of hydrogen from Mars.

Published
2022

29. 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

30. Climatology of the CO vertical distribution on Mars based on ACS TGO measurements

Author

Fedorova, Anna A., primary, Trokhimovskiy, Alexander, additional, Lefèvre, Franck, additional, Olsen, Kevin S., additional, Korablev, Oleg I, additional, Montmessin, Franck, additional, Ignatiev, Nikolay I., additional, Lomakin, Alexander A, additional, Forget, Francois, additional, Belyaev, Denis A., additional, Alday, Juan, additional, Luginin, Mikhail, additional, Patrakeev, Andrey, additional, Shakun, Alexey V., additional, and Grigoriev, Alexey, additional

Published
2022
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31. Isotopic Composition of CO 2 in the Atmosphere of Mars: Fractionation by Diffusive Separation Observed by the ExoMars Trace Gas Orbiter

Author

Alday, Juan, primary, Wilson, Colin F., additional, Irwin, Patrick G. J., additional, Trokhimovskiy, Alexander, additional, Montmessin, Franck, additional, Fedorova, Anna A., additional, Belyaev, Denis A., additional, Olsen, Kevin S., additional, Korablev, O., additional, Lefèvre, Franck, additional, Braude, Ashwin S., additional, Baggio, Lucio, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2021
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32. A Two‐Martian Years Survey of the Water Vapor Saturation State on Mars Based on ACS NIR/TGO Occultations.

Author

Fedorova, Anna, Montmessin, Franck, Trokhimovskiy, Alexander, Luginin, Mikhail, Korablev, Oleg, Alday, Juan, Belyaev, Denis, Holmes, James, Lefevre, Franck, Olsen, Kevin, Patrakeev, Andrey, and Shakun, Alexey

Subjects
ATMOSPHERIC chemistry, WATER vapor, ATMOSPHERIC boundary layer, MARTIAN atmosphere, NEAR infrared radiation, MARS (Planet), DUST storms
Abstract

On Mars, condensation is the major factor constraining the vertical distribution of water vapor. Recent measurements of water and temperature profiles showed that water can be strongly supersaturated at and above the level where clouds form during the aphelion and perihelion seasons. Since 2018, the near‐infrared spectrometer (NIR) of the Atmospheric Chemistry Suite onboard the Trace Gas Orbiter has measured H2O and temperature profiles using solar occultation in the infrared from below 10 to 100 km of altitude. Here, we provide the first long‐term monitoring of the water saturation state. The survey spans 2 Martian years from Ls = 163° of MY34 to Ls = 170° of MY36. We found that water is often supersaturated above aerosol layers. In the aphelion season, the water mixing ratio above 40 km in the mid‐to‐high latitudes was below 3 ppmv and yet is found to be supersaturated. Around the perihelion, water is also supersaturated above 60 km with a mixing ratio of 30–50 ppmv. Stronger saturation is observed during the dusty season in MY35 compared to what was observed in MY34 during the Global Dust Storm and around the perihelion. Saturation varied between the evening and morning terminators in response to temperature modulation imparted by thermal tides. Although water vapor is more abundant in the evening, colder morning temperatures induce a daily peak of saturation. This data set establishes a new paradigm for water vapor on Mars, revealing that supersaturation is nearly ubiquitous, particularly during the dust season, thereby promoting water escape on an annual average. Plain Language Summary: The rate of water loss from Mars depends on hydrogen, the main product of the H2O photodissociation escaping from the upper atmosphere. The ability of water to reach high altitudes and to be a direct source of atomic hydrogen is limited by cloud formation, which holds water vapor in the lower atmosphere. This process is regulated by temperature and pressure. Condensation starts when the temperature is cold enough and condensation nuclei (CN) (e.g., small dust particles) are available. If CN are lacking, or their sizes are too small, or the temperature drops too fast, then water vapor becomes supersaturated. Recent studies have shown that Martian water vapor is often supersaturated. Here, we present the first seasonal cycle of the saturation state from simultaneous measurements of water and temperature during two Martian years by Atmospheric Chemistry Suite on the Trace Gas Orbiter. Our results show that supersaturation is typical on Mars. It occurs above clouds both in the aphelion and perihelion seasons as well as in the lower polar atmosphere. We demonstrate supersaturation to be an important factor facilitating the escape of water. Unlike the Earth, water easily penetrates the upper atmosphere and reaches photodissociation altitudes. Key Points: Long‐term observations of H2O saturation state in the atmosphere of Mars show that supersaturation is nearly ubiquitous above aerosol layersDuring the dusty season, the supersaturation is stronger in MY35 compared to MY34More water was found in the evening terminator and stronger supersaturation in the morning terminator [ABSTRACT FROM AUTHOR]

Published
2023
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33. Thermal tides in Martian atmosphere from ACS/TIRVIM

Author

Fan, Siteng, primary, Guerlet, Sandrine, additional, Forget, Francois, additional, Bierjon, Antoine, additional, Millour, Ehouarn, additional, Ignatiev, Nikolay, additional, Shakun, Alexey, additional, Grigoriev, Alexey, additional, Trokhimovskiy, Alexander, additional, Montmessin, Franck, additional, and Korablev, Oleg, additional

Published
2021
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34. Martian atmospheric thermal structures and dust distributions during the global dust storm and the regional dust storm of MY 34 from ACS TIRVIM observations onboard ExoMars TGO

Author

Vlasov, Pavel, primary, Ignatiev, Nikolay, additional, Guerlet, Sandrine, additional, Grassi, Davide, additional, Grigoriev, Аlexey, additional, Shakun, Alexey, additional, Patsaev, Dmitriy, additional, Maslov, Igor, additional, Luginin, Michail, additional, Millour, Ehouarn, additional, Forget, François, additional, Arnold, Gabriele, additional, Trokhimovskiy, Аlexander, additional, Korablev, Oleg, additional, and Montmessin, Franck, additional

Published
2021
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37. The distribution and saturation of water vapor with ACS/TGO for first Martian year of observations

Author

Fedorova, Anna, Montmessin, Franck, Korablev, Oleg, Luginin, Mikhail, Trokhimovskiy, Alexander, Belyaev, Denis, Alday, Juan, Ignatiev, Nikolay, Lefèvre, Franck, Olsen, Kevin, Millour, Ehouarn, Bertaux, Jean-Loup, Shakun, Alexey, Grigoriev, Alexey, Patrakeev, Andrey, Korsa, Svyatoslav, Wilson, Colin, Forget, François, Määttänen, Anni, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), 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), Department of Physics [Oxford], University of Oxford [Oxford], 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), and Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP)

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

International audience; The water vapour vertical distribution is an eloquent gauge of the relative roles of the various sources, sinks and processes that control the Martian water cycle. However, its behaviour is still poorly studied while it is instrument for our understanding of the loss of water from Mars to space, which results from the transport of water to the upper atmosphere where it is disassociated to hydrogen atoms that later escape. We use the Atmospheric Chemistry Suite on the ExoMars Trace Gas Orbiter to characterize the water distribution with altitude. Here we present results of the Atmospheric Chemistry Suite (ACS) instrument NIR channel for the first year of TGO observations covering the almost full year from Ls 160° of the Martian year 34 (April 2018) to Ls 130° of the Martian year 35 (January 2020). Simultaneous measurements of the water vapour mixing ratio, temperature and dust vertical distribution and formation of water ice clouds allow us to constrain the complex water behaviour and estimate the saturation state of H2O. Water profiles during the 2018-2019 southern spring and summer stormy seasons show that high altitude water is preferentially supplied close to perihelion and that large supersaturation occurs even when clouds are present. Here we attempt to complete the story by studying water vapor during the northern spring and summer to explore whether saturation impacts water transport between hemispheres in this season. The data analysis of MY35 was supported by RSF (project No. 20-42-09035).

Published
2020

38. Transient HCl in the atmosphere of Mars

Author

Korablev, Oleg, primary, Olsen, Kevin S., additional, Trokhimovskiy, Alexander, additional, Lefèvre, Franck, additional, Montmessin, Franck, additional, Fedorova, Anna A., additional, Toplis, Michael J., additional, Alday, Juan, additional, Belyaev, Denis A., additional, Patrakeev, Andrey, additional, Ignatiev, Nikolay I., additional, Shakun, Alexey V., additional, Grigoriev, Alexey V., additional, Baggio, Lucio, additional, Abdenour, Irbah, additional, Lacombe, Gaetan, additional, Ivanov, Yury S., additional, Aoki, Shohei, additional, Thomas, Ian R., additional, Daerden, Frank, additional, Ristic, Bojan, additional, Erwin, Justin T., additional, Patel, Manish, additional, Bellucci, Giancarlo, additional, Lopez-Moreno, Jose-Juan, additional, and Vandaele, Ann C., additional

Published
2021
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39. Photolysis controls the isotopic composition of water products escaping Mars’ atmosphere

Author

Alday, Juan, primary, Trokhimovskiy, Alexander, additional, Irwin, Patrick, additional, Wilson, Colin, additional, Montmessin, Franck, additional, Lefèvre, Franck, additional, Fedorova, Anna, additional, Belyaev, Denys, additional, Olsen, Kevin, additional, Korablev, Oleg, additional, Vals, Margaux, additional, Rossi, Loïc, additional, Baggio, Lucio, additional, Bertaux, Jean-Loup, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2021
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40. HCl in the atmosphere of Mars: first detection of a halide gas

Author

Olsen, Kevin S., primary, Trokhimovskiy, Alexander, additional, Korablev, Oleg, additional, Lefèvre, Franck, additional, Montmessin, Franck, additional, Fedorova, Anna A., additional, Alday, Juan, additional, Belyaev, Denis A., additional, Lucio, Baggio, additional, Patrakeev, Andrey, additional, Grigoriev, Alexey, additional, and Shakun, Alexey, additional

Published
2020
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41. Hunting for Methane on Mars: one Martian year of survey with ACS on TGO

Author

Montmessin, Franck, primary, Korablev, Oleg, additional, Fedorova, Anna A., additional, Trokhimovskiy, Alexander V., additional, Lefevre, Franck, additional, Baggio, Lucio, additional, Belyaev, Denis A., additional, Olsen, Kevin, additional, Alday, Juan, additional, Irbah, Abdenour, additional, Lacombe, Gaetan, additional, Patrakeev, Andrey, additional, Teinturier, Lucas, additional, Ignatiev, Nikolay, additional, Luginin, Mikhail, additional, Shakun, Alexey, additional, Guerlet, Sandrine, additional, Forget, François, additional, Millour, Ehouarn, additional, and Wilson, Colin F., additional

Published
2020
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42. Isotopic composition of water vapour in the Martian atmosphere: vertical profiles from ACS MIR on ExoMars TGO

Author

Alday, Juan, primary, Irwin, Patrick G. J., additional, Wilson, Colin F., additional, Olsen, Kevin S., additional, Baggio, Lucio, additional, Montmessin, Franck, additional, Korablev, Oleg, additional, Trokhimovskiy, Alexander, additional, Fedorova, Anna A., additional, Belyaev, Denis A., additional, Shakun, Alexey, additional, Patrakeev, Andrew, additional, and Grigoriev, Alexey, additional

Published
2020
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43. HCl in the atmosphere of Mars: chlorine isotopic ratio

Author

Trokhimovskiy, Alexander, primary, Olsen, Kevin, additional, Korablev, Oleg, additional, Montmessin, Franck, additional, Lefevre, Franck, additional, Fedorova, Anna, additional, Alday Parejo, Juan, additional, Beliaev, Denis, additional, Patrakeev, Andrey, additional, and Shakun, Alexey, additional

Published
2020
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46. The distribution and saturation of water vapor as inferred from ACS during the first Martian year of TGO Science observations

Author

Fedorova, Anna, primary, Montmessin, Franck, additional, Korablev, Oleg, additional, Luginin, Mikhail, additional, Trokhimovskiy, Alexander, additional, Belyaev, Denis, additional, Alday, Juan, additional, Ignatiev, Nikolay, additional, Lefevre, Franck, additional, Olsen, Kevin, additional, Millour, Ehouarn, additional, Bertaux, Jean-Loup, additional, Shakun, Alexey, additional, Grigoriev, Alexey, additional, Patrakeev, Andrey, additional, Korsa, Svyatoslav, additional, Wilson, Colin, additional, Forget, Francois, additional, and Maattanen, Anna, additional

Published
2020
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47. Stormy water on Mars: The distribution and saturation of atmospheric water during the dusty season

Author

Fedorova, Anna A., primary, Montmessin, Franck, additional, Korablev, Oleg, additional, Luginin, Mikhail, additional, Trokhimovskiy, Alexander, additional, Belyaev, Denis A., additional, Ignatiev, Nikolay I., additional, Lefèvre, Franck, additional, Alday, Juan, additional, Irwin, Patrick G. J., additional, Olsen, Kevin S., additional, Bertaux, Jean-Loup, additional, Millour, Ehouarn, additional, Määttänen, Anni, additional, Shakun, Alexey, additional, Grigoriev, Alexey V., additional, Patrakeev, Andrey, additional, Korsa, Svyatoslav, additional, Kokonkov, Nikita, additional, Baggio, Lucio, additional, Forget, Francois, additional, and Wilson, Colin F., additional

Published
2020
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48. Isotopic Composition of CO2 in the Atmosphere of Mars: Fractionation by Diffusive Separation Observed by the ExoMars Trace Gas Orbiter.

Author

Alday, Juan, Wilson, Colin F., Irwin, Patrick G. J., Trokhimovskiy, Alexander, Montmessin, Franck, Fedorova, Anna A., Belyaev, Denis A., Olsen, Kevin S., Korablev, O., Lefèvre, Franck, Braude, Ashwin S., Baggio, Lucio, Patrakeev, Andrey, and Shakun, Alexey

Subjects
ISOTOPES, ATMOSPHERIC carbon dioxide, PLANETARY atmospheres, ATMOSPHERIC chemistry, MARS (Planet)
Abstract

Isotopic ratios in atmospheric CO2 are shaped by various processes throughout Mars' history, and can help understand what the atmosphere of early Mars was like to sustain liquid water on its surface. In this study, we monitor the O and C isotopic composition of CO2 between 70 and 130 km for more than half a Martian year using solar occultation observations by the Atmospheric Chemistry Suite onboard the ExoMars Trace Gas Orbiter. We find the vertical trends of the isotopic ratios to be consistent with the expectations from diffusive separation above the homopause, with average values below this altitude being consistent with Earth‐like fractionation (δ13C = −3 ± 37‰; δ18O = −29 ± 38‰; and δ17O = −11 ± 41‰). Using these measurements, we estimate that at least 20%–40% of primordial C on Mars has escaped to space throughout history. The total amount of C lost from the atmosphere is likely to be well in excess of this lower limit, due to carbonate formation and further sink processes. In addition, we propose a photochemical transfer of light O from H2O to CO2 to explain the larger enrichment in the O18/O16 ${}^{18}\mathrm{O}/{}^{16}\mathrm{O}$ ratio in H2O than in CO2. Plain Language Summary: There is ample evidence suggesting that liquid water was abundant on the surface of Mars in the past. However, climatic conditions on early Mars must have been very different from the ones we observe today to sustain liquid water on its surface. The ratios of the heavy and light isotopes in different species provide a very useful tool to estimate the early climate of Mars. In this study, we monitor the isotopic ratios of carbon dioxide in the atmosphere of Mars to provide more accurate estimates of these. With our measurements, and in context with previous studies, we estimate that at least 20%–40% of the carbon reservoir has been lost to space throughout Martian history. This, together with the sequestration of atmospheric C on the surface in the form of minerals, is consistent with the idea that the atmosphere of early Mars was denser than the one we observe today. Key Points: Isotopic ratios in CO2 are observed to be consistent with telluric standards and to fractionate by diffusive separation above the homopauseAt least 20%–40% of the C reservoir has escaped to space throughout Martian historyThe higher 18O/16O ratio in H2O than in CO2 may be explained by a photochemical transfer of lighter O from H2O to CO2 [ABSTRACT FROM AUTHOR]

Published
2021
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49. 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

50. Thermal structure and aerosol content in the martian atmosphere from ACS-TIRVIM on board ExoMars/TGO

Author

Guerlet, Sandrine, Ignatiev, Nikolay, Forget, François, Fouchet, Thierry, Shakun, Alexey, Millour, Ehouarn, Montabone, Luca, Young, Roland, Grigoriev, Alexey, Trokhimovskiy, Alexander, Montmessin, Franck, Korablev, Oleg, 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), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), 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), Space Science Institute [Boulder] (SSI), 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), 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), 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), and Guerlet, Sandrine

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 ExoMars Trace Gas Orbiter (TGO), a mission by ESA and Roscosmos, was launched in March 2016 and reached its final, near-circular 400 km orbit around Mars in March, 2018. On board TGO, the Atmospheric Chemistry Suite (ACS) is a set of three spectrometers including a thermal-infrared channel, TIRVIM. This Fourier-transform spectrometer covers the range 600-6000 cm-1 (1.7-17μm) with a spectral resolution of 1.2 cm-1. We focus here on nadir observations in the range 600-1300 cm-1, which covers absorption by CO2 (centered at 667 cm-1), water ice clouds (centered at 820 cm-1) and dust (centered at 1100 cm-1). The advantage of the TIRVIM data set over previous instruments comes from the TGO orbit, which is not sun-synchronous and was designed to sample a complete daily cycle every 55 days. Hence, TIRVIM has the capacity to uniquely study both the diurnal and seasonal variability of the thermal structure, dust and ice cloud opacity. We have developed a radiative transfer model coupled to a retrieval algorithm that exploits TIRVIM spectra to simultaneously retrieve vertical profiles of the temperature from 5 to 45 km, surface temperature, and integrated optical depth of dust and water ice clouds. This algorithm was tested and validated against synthetic observations generated under various conditions (local time, seasons, latitude, aerosol load, ...). We have then applied this algorithm to the first 45 days of TIRVIM data acquired in March-April, 2018. The retrieved temperature profiles have been validated against thousands of co-located measurements acquired by the Mars Climate Sounder around 3am and 3pm, a limb-viewing radiometer onboard Mars Reconnaissance Orbiter. The agreement between the two data sets is very satisfactory. In particular, the amplitude of the diurnal thermal tide as seen by MCS is very well captured by TIRVIM at pressures greater than 10 Pa. However, TIRVIM underestimates it in the range 1-10 Pa, which is due to a much poorer vertical resolution in this region (as expected from a nadir-viewing sounder). We will present these results with an emphasis on the diurnal cycle of the atmospheric temperature and the aerosols load, along with comparisons with predictions from the LMD Mars GCM. Analysis of TIRVIM data acquired during the dust storm in June-July 2018 is in progress and will also be presented. Acknowledgements: The ACS experiment is led by IKI in Moscow. We acknowledge support by CNES and Roscosmos.

Published
2019

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