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1. Strong variability of Martian water ice clouds during dust storms revealed from ExoMars Trace Gas Orbiter/NOMAD

Author

Liuzzi, Giuliano, Villanueva, Geronimo L., Crismani, Matteo M. J., Smith, Michael D., Mumma, Michael J., Daerden, Frank, Aoki, Shohei, Vandaele, Ann Carine, Clancy, R. Todd, Erwin, Justin, Thomas, Ian, Ristic, Bojan, Lopez-Moreno, José-Juan, Bellucci, Giancarlo, and Patel, Manish R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Observations of water ice clouds and aerosols on Mars can provide important insights into the complexity of the water cycle. Recent observations have indicated an important link between dust activity and the water cycle, as intense dust activity can significantly raise the hygropause, and subsequently increase the escape of water after dissociation in the upper atmosphere. Here present observations from NOMAD/TGO that investigate the variation of water ice clouds in the perihelion season of Mars Year 34 (April 2018-19), their diurnal and seasonal behavior, and the vertical structure and microphysical properties of water ice and dust. These observations reveal the recurrent presence of a layer of mesospheric water ice clouds subsequent to the 2018 Global Dust Storm. We show that this layer rose from 45 to 80 km in altitude on a timescale of days from heating in the lower atmosphere due to the storm. In addition, we demonstrate that there is a strong dawn dusk asymmetry in water ice abundance, related to nighttime nucleation and subsequent daytime sublimation. Water ice particle sizes are retrieved consistently and exhibit sharp vertical gradients (from 0.1 to 4.0 um), as well as mesospheric differences between the Global Dust Storm (<0.5 um) and the 2019 regional dust storm (1.0 um), which suggests differing water ice nucleation efficiencies. These results form the basis to advance our understanding of mesospheric water ice clouds on Mars, and further constrain the interactions between water ice and dust in the middle atmosphere., Comment: Submitted to Journal of Geophysical Research - Planets. 36 pages, 9 figures, 1 table

Published
2019
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4. First Detection and Thermal Characterization of Terminator CO 2 Ice Clouds With ExoMars/NOMAD

Author

Liuzzi, Giuliano, primary, Villanueva, Geronimo L., additional, Trompet, Loïc, additional, Crismani, Matteo M. J., additional, Piccialli, Arianna, additional, Aoki, Shohei, additional, Lopez‐Valverde, Miguel Angel, additional, Stolzenbach, Aurélien, additional, Daerden, Frank, additional, Neary, Lori, additional, Smith, Michael D., additional, Patel, Manish R., additional, Lewis, Stephen R., additional, Clancy, R. Todd, additional, Thomas, Ian R., additional, Ristic, Bojan, additional, Bellucci, Giancarlo, additional, Lopez‐Moreno, Jose‐Juan, additional, and Vandaele, Ann Carine, additional

Published
2021
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5. Probing the Atmospheric Cl Isotopic Ratio on Mars: Implications for Planetary Evolution and Atmospheric Chemistry

Author

Liuzzi, Giuliano, primary, Villanueva, Geronimo L., additional, Viscardy, Sebastien, additional, Mège, Daniel, additional, Crismani, Matteo M. J., additional, Aoki, Shohei, additional, Gurgurewicz, Joanna, additional, Tesson, Pierre‐Antoine, additional, Mumma, Michael J., additional, Smith, Michael D., additional, Faggi, Sara, additional, Kofman, Vincent, additional, Knutsen, Elise W., additional, Daerden, Frank, additional, Neary, Lori, additional, Schmidt, Frédéric, additional, Trompet, Loïc, additional, Erwin, Justin T., additional, Robert, Séverine, additional, Thomas, Ian R., additional, Ristic, Bojan, additional, Bellucci, Giancarlo, additional, Lopez‐Moreno, Jóse Juan, additional, Patel, Manish R., additional, and Vandaele, Ann Carine, additional

Published
2021
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6. Comprehensive investigation of Mars methane and organics with ExoMars/NOMAD

Author

Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), UK Space Agency, National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Agenzia Spaziale Italiana, Knutsen, Elise W., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M. J., Mumma, Michael J., Smith, Michael D., Vandaele, Ann Carine, Aoki, Shohei, Thomas, Ian R., Daerden, Frank, Viscardy, Sébastien, Erwin, Justin T., Trompet, Loic, Neary, Lori, Ristic, Bojan, López-Valverde, M. A., López-Moreno, José Juan, Patel, Manish R., Karatekin, Ozgur, Bellucci, Giancarlo, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), UK Space Agency, National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Agenzia Spaziale Italiana, Knutsen, Elise W., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M. J., Mumma, Michael J., Smith, Michael D., Vandaele, Ann Carine, Aoki, Shohei, Thomas, Ian R., Daerden, Frank, Viscardy, Sébastien, Erwin, Justin T., Trompet, Loic, Neary, Lori, Ristic, Bojan, López-Valverde, M. A., López-Moreno, José Juan, Patel, Manish R., Karatekin, Ozgur, and Bellucci, Giancarlo

Abstract

Methane (CH4) on Mars has attracted a great deal of attention since it was first detected in January 2003. As methane is considered a potential marker for past/present biological or geological activity, any possible detection would require evidence with strong statistical significance. Ethane (C2H6) and ethylene (C2H4) are also relevant chemical species as their shorter lifetimes in the Martian atmosphere make them excellent tracers for recent and ongoing releases. If detected, a CH4/C2Hn ratio could aid in constraining the potential source of organic production. Here we present the results of an extensive search for hydrocarbons in the Martian atmosphere in 240,000 solar occultation measurements performed by the ExoMars Trace Gas Orbiter/NOMAD instrument from April 2018 to April 2019. The observations are global, covering all longitudes and latitudes from 85°N to 85°S, and sampled from 6 to 100 km altitude with a typical vertical resolution of 2 km. There were no statistically significant detections of organics and new stringent upper limits for global ethane and ethylene were set at 0.1 ppbv and 0.7 ppbv, respectively. No global background level of methane was observed, obtaining an upper limit of 0.06 ppbv, in agreement with early results from ExoMars (Korablev et al., 2019). Dedicated searches for localized plumes at more than 2000 locations provided no positive detections, implying that if methane were released in strong and rapid events, the process would have to be sporadic. © 2020 Elsevier Inc. All rights reserved.

Published
2021

7. Probing the Atmospheric Cl Isotopic Ratio on Mars: Implications for Planetary Evolution and Atmospheric Chemistry

Author

Belgian Science Policy Office, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), UK Space Agency, National Aeronautics and Space Administration (US), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Agenzia Spaziale Italiana, European Space Agency, Liuzzi, Giuliano, Villanueva, Geronimo L., Viscardy, Sebastien, Mège, Daniel, Crismani, Matteo M. J., Aoki, Shohei, Gurgurewicz, Joanna, Tesson, Pierre-Antoine, Mumma, Michael J., Smith, Michael D., Faggi, Sara, Kofman, Vincent, Knutsen, Elise W., Daerden, Frank, Neary, Lori, Schmidt, Frédéric, Trompet, Loïc., Erwin, Justin T., Robert, Séverine, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, López-Moreno, José Juan, Patel, Manish R., Vandaele, Ann Carine, Belgian Science Policy Office, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), UK Space Agency, National Aeronautics and Space Administration (US), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Agenzia Spaziale Italiana, European Space Agency, Liuzzi, Giuliano, Villanueva, Geronimo L., Viscardy, Sebastien, Mège, Daniel, Crismani, Matteo M. J., Aoki, Shohei, Gurgurewicz, Joanna, Tesson, Pierre-Antoine, Mumma, Michael J., Smith, Michael D., Faggi, Sara, Kofman, Vincent, Knutsen, Elise W., Daerden, Frank, Neary, Lori, Schmidt, Frédéric, Trompet, Loïc., Erwin, Justin T., Robert, Séverine, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, López-Moreno, José Juan, Patel, Manish R., and Vandaele, Ann Carine

Abstract

Following the recent detection of HCl in the atmosphere of Mars by ExoMars/Trace Gas Orbiter, we present here the first measurement of the 37Cl/35Cl isotopic ratio in the Martian atmosphere using a set of Nadir Occultation for MArs Discovery (NOMAD) observations. We determine an isotopic anomaly of −6 ± 78‰ compared to Earth standard, consistent with the −51‰–−1‰ measured on Mars’ surface by Curiosity. The measured isotopic ratio is also consistent with surface measurements, and suggests that Cl reservoirs may have undergone limited processing since formation in the Solar Nebula. The examination of possible sources and sinks of HCl shows only limited pathways to short-term efficient Cl fractionation and many plausible reservoirs of “light” Cl. © 2021. American Geophysical Union.

Published
2021

8. Strong Variability of Martian Water Ice Clouds During Dust Storms Revealed From ExoMars Trace Gas Orbiter/NOMAD

Author

Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), National Aeronautics and Space Administration (US), Liuzzi, Giuliano, Villanueva, Geronimo L., Crismani, Matteo M. J., Smith, Michael D., Mumma, Michael J., Daerden, Frank, Aoki, Shohei, Vandaele, Ann Carine, Clancy, R. Todd, Erwin, Justin T., Thomas, Ian R., Ristic, Bojan, López-Moreno, José Juan, Bellucci, Giancarlo, Patel, Manish R., Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), National Aeronautics and Space Administration (US), Liuzzi, Giuliano, Villanueva, Geronimo L., Crismani, Matteo M. J., Smith, Michael D., Mumma, Michael J., Daerden, Frank, Aoki, Shohei, Vandaele, Ann Carine, Clancy, R. Todd, Erwin, Justin T., Thomas, Ian R., Ristic, Bojan, López-Moreno, José Juan, Bellucci, Giancarlo, and Patel, Manish R.

Abstract

Observations of water ice clouds and aerosols on Mars can provide important insights into the complexity of the water cycle. Recent observations have indicated an important link between dust activity and the water cycle, as intense dust activity can significantly raise the hygropause, and subsequently increase the escape of water after dissociation in the upper atmosphere. Here present observations from Nadir and Occultation for MArs Discovery/Trace Gas Orbiter that investigate the variation of water ice clouds in the perihelion season of Mars year 34 (April 2018-2019), their diurnal and seasonal behavior, and the vertical structure and microphysical properties of water ice and dust. These observations reveal the recurrent presence of a layer of mesospheric water ice clouds subsequent to the 2018 global dust storm. We show that this layer rose from 45 to 80 km in altitude on a time scale of days from heating in the lower atmosphere due to the storm. In addition, we demonstrate that there is a strong dawn-dusk asymmetry in water ice abundance, related to nighttime nucleation and subsequent daytime sublimation. Water ice particle sizes are retrieved consistently and exhibit sharp vertical gradients (from 0.1 to 4.0 mu m), as well as mesospheric differences between the global dust storm (<0.5 mu m) and the 2019 regional dust storm (1.0 mu m), which suggests differing water ice nucleation efficiencies. These results form the basis to advance our understanding of mesospheric water ice clouds on Mars, and further constrain the interactions between water ice and dust in the middle atmosphere. © 2020 American Geophysical Union

Published
2020

9. First Detection and Thermal Characterization of Terminator CO2 Ice Clouds With ExoMars/NOMAD.

Author

Liuzzi, Giuliano, Villanueva, Geronimo L., Trompet, Loïc, Crismani, Matteo M. J., Piccialli, Arianna, Aoki, Shohei, Lopez‐Valverde, Miguel Angel, Stolzenbach, Aurélien, Daerden, Frank, Neary, Lori, Smith, Michael D., Patel, Manish R., Lewis, Stephen R., Clancy, R. Todd, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Lopez‐Moreno, Jose‐Juan, and Vandaele, Ann Carine

Subjects
ICE clouds, TRACE gases, MARTIAN atmosphere, ICE nuclei, UPPER atmosphere, FREEZING points
Abstract

We present observations of terminator CO2 ice clouds events in three groups: Equatorial dawn, Equatorial dusk (both between 20°S and 20°N) and Southern midlatitudes at dawn (45°S and 55°S east of Hellas Basin) with ESA ExoMars Trace Gas Orbiter's Nadir and Occultation for MArs Discovery instrument. CO2 ice abundance is retrieved simultaneously with water ice, dust, and particle sizes, and rotational temperature and CO2 column profiles in 16 of 26 cases. Small particles (<0.5 μm) prevail at dusk, while water ice likely provides most source nuclei at dawn. Clouds east of Hellas are found to be dominantly nucleated on surface‐lifted dust. CO2 ice is sometimes detected in unsaturated air together with dust nuclei at dawn, suggesting ongoing sublimation. Depending on latitude and local time, the interplay between particle precipitation and the lifetime of temperature minima (i.e., cold pockets) determines CO2 ice properties. Plain Language Summary: The upper atmosphere of Mars is characterized by the seasonal presence of CO2 ice clouds. Their properties have been long studied, as well as their formation mechanisms in relation to the thermal structure of the atmosphere and its variability. In this study, we present the first observations of these clouds at the terminator (dawn and dusk) by the NOMAD spectrometer onboard the Exomars Trace Gas Orbiter. CO2 ice is detected simultaneously with dust, water ice and the temperature profile. Our results agree with previous findings in terms of how clouds are spatially distributed and their temporal occurrence. However, we also explore the sources of condensation nuclei for CO2 ice particles, showing that water ice is a possible source at dawn near the Equator. We also identify surface‐lifted dust below the CO2 ice clouds observed east of Hellas Basin, suggesting that, at that location, dust could provide nuclei for CO2 ice. CO2 ice is also sometimes detected at temperatures higher than the CO2 freezing point, suggesting ongoing sublimation. In this work we explore for the first time the composition of CO2 ice clouds, which is critical to advance our understanding of how CO2 ice clouds form in the mesosphere at Mars. Key Points: Twenty Six mesospheric CO2 ice clouds were detected with NOMAD SO in Mars Year 35, simultaneously with water ice, dust, and CO2 saturation ratiosEquatorial CO2 clouds are observed at 50–80 km altitude at dusk, and 40–60 km at dawn, when water ice likely provides condensation nucleiSix CO2 ice clouds are found east of Hellas basin; their formation is likely sourced by surface‐lifted dust at 40–65 km [ABSTRACT FROM AUTHOR]

Published
2021
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10. Variability of D and H in the Martian Exosphere

Author

Clarke, John T., Mayyasi, Majd, Bhattacharyya, Dolon, McCord Schneider, Nicholas, Mcclintock, Bill, Deighan, Justin, Stewart, Ian F., Chaufray, Jean-Yves, Chaffin, Michael, Jain, Sonal K., Stiepen, Arnaud, Crismani, Matteo M. J., Holsclaw, Greg, Montmessin, Franck, Jakosky, Bruce Martin, Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), University of Colorado [Boulder], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), 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), PLANETO - LATMOS, and Cardon, Catherine

Subjects
[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.PHYS.PHYS-AO-PH] Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; The IUVS instrument on MAVEN contains an echelle spectrograph with a novel optical design to enable long-aperture measurements of emission lines in the absence of continuum, intended primarily to measure the H and D Ly α emission lines from the martian upper atmosphere. The main scientific goal of the echelle channel is to measure the H and D Ly α emissions that result from resonant scattering of solar emission and to discover how the H and D densities, temperatures, and escape fluxes vary with location, season, topography, etc. The global D/H ratio of the martian atmosphere is roughly 5 times higher than in the terrestrial atmosphere due to the escape of a large volume of water into space, likely early in the history of Mars. Since H atoms escape faster than D atoms, the D/H ratio increases with time as more water is lost. Earth-based IR observations have indicated large variations in the HDO/H2O ratio in the lower atmosphere from location to location, and possible changes with the atmospheric seasonal cycles [Villanueva et al. 2015]. HST and MEX measurements of the H corona of Mars have shown large (order of magnitude) changes in the H exosphere and escape flux with changing seasons and/or heliospheric distance [Clarke et al. 2014; Chaffin et al. 2014]. A series of observations of D and H with the IUVS echelle channel now show a strong trend in the variation of both emissions, with order of magnitude changes in both species in the upper atmosphere. With the added data expected in Fall 2016, we will be able to determine this trend over a full range of martian solar longitude. These results and a comparison with proposed processes that might lead to the observed changes will be presented.

Published
2016

11. New Observations of Molecular Nitrogen by the Imaging Ultraviolet Spectrograph on MAVEN

Author

Stevens, Michael H., Evans, J. Scott, Schneider, Nicholas M., Stewart, A. Ian F., Deighan, Justin, Jain, Sonal K., Crismani, Matteo M. J., Stiepen, Arnaud, Chaffin, Michael S., Mcclintock, William E., Holsclaw, Greg M., Lefèvre, Franck, Montmessin, Franck, Lo, Daniel Y., Clarke, John T., Bougher, Stephen W., Jakosky, Bruce M., Naval Research Laboratory (NRL), Computational Physics, Inc., Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], 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), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, and Cardon, Catherine

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

International audience; The Martian ultraviolet dayglow provides information on the basic state of the Martian upper atmosphere. The Imaging Ultraviolet Spectrograph (IUVS) on NASA’s Mars Atmosphere and Volatile Evolution (MAVEN) mission has observed Mars at mid and far-UV wavelengths since its arrival in September 2014. In this work, we describe a linear regression method used to extract components of UV spectra from IUVS limb observations and focus in particular on molecular nitrogen (N2) photoelectron excited emissions. We identify N2 Lyman-Birge-Hopfield (LBH) emissions for the first time at Mars and we also confirm the tentative identification of N2 Vegard-Kaplan (VK) emissions. We compare observed VK and LBH limb radiance profiles to model results between 90 and 210 km. Finally, we compare retrieved N2 density profiles to general circulation (GCM) model results. Contrary to earlier analyses using other satellite data that indicated N2 densities were a factor of three less than predictions, we find that N2 abundances exceed GCM results by about a factor of two at 130 km but are in agreement at 150 km.

Published
2015

12. Non-Migrating Tides in the Martian Atmosphere as Observed by MAVEN IUVS

Author

Lo, Daniel Y., Yelle, Roger V., Schneider, Nicholas M., Jain, Sonal K., Stewart, A. Ian F., England, Scott L., Deighan, Justin I., Stiepen, Arnaud, Evans, J. Scott, Stevens, Michael H., Chaffin, Michael S., Crismani, Matteo M. J., Mcclintock, William E., Clarke, John T., Holsclaw, Gregory M., Lefèvre, Franck, Jakosky, Bruce M., Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Naval Research Laboratory (NRL), Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)

Subjects
[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], upper atmosphere, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars, MAVEN/IUVS, atmospheric tides, CO2 density
Abstract

International audience; Using the Mars Atmospheric and Volatile EvolutioN mission (MAVEN) Imaging Ultraviolet Spectrograph (IUVS), we found periodic longitudinal variations in CO2 density in the Martian atmosphere. The variations exhibit significant structure with longitudinal wave numbers 1, 2, and 3 in an effectively constant local solar time frame, and we attribute this structure to nonmigrating tides. The wave-2 component is dominated by the diurnal eastward moving DE1 tide at the equator and the semidiurnal stationary S0 tide at the midlatitudes. Wave-3 is dominated by the diurnal eastward moving DE2 tide, with possibly the semidiurnal eastward moving SE1 tide causing an amplitude increase at the midlatitudes. Structure in the wave-1 component can be explained by the semidiurnal westward moving SW1 tide.

Published
2015

13. Nonmigrating tides in the Martian atmosphere as observed by MAVEN IUVS

Author

Lo, Daniel Y., primary, Yelle, Roger V., additional, Schneider, Nicholas M., additional, Jain, Sonal K., additional, Stewart, A. Ian F., additional, England, Scott L., additional, Deighan, Justin I., additional, Stiepen, Arnaud, additional, Evans, J. Scott, additional, Stevens, Michael H., additional, Chaffin, Michael S., additional, Crismani, Matteo M. J., additional, McClintock, William E., additional, Clarke, John T., additional, Holsclaw, Gregory M., additional, Lefèvre, Franck, additional, and Jakosky, Bruce M., additional

Published
2015
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14. Ultraviolet observations of the hydrogen coma of comet C/2013 A1 (Siding Spring) by MAVEN/IUVS

Author

Crismani, Matteo M. J., primary, Schneider, Nicholas M., additional, Deighan, Justin I., additional, Stewart, A. Ian F., additional, Combi, Michael, additional, Chaffin, Michael S., additional, Fougere, Nicolas, additional, Jain, Sonal K., additional, Stiepen, Arnaud, additional, Yelle, Roger V., additional, McClintock, William E., additional, Clarke, John T., additional, Holsclaw, Gregory M., additional, Montmessin, Frank, additional, and Jakosky, Bruce M., additional

Published
2015
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15. First Detection and Thermal Characterization of Terminator CO2Ice Clouds With ExoMars/NOMAD

Author

Liuzzi, Giuliano, Villanueva, Geronimo L., Trompet, Loïc, Crismani, Matteo M. J., Piccialli, Arianna, Aoki, Shohei, Lopez‐Valverde, Miguel Angel, Stolzenbach, Aurélien, Daerden, Frank, Neary, Lori, Smith, Michael D., Patel, Manish R., Lewis, Stephen R., Clancy, R. Todd, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Lopez‐Moreno, Jose‐Juan, and Vandaele, Ann Carine

Abstract

We present observations of terminator CO2ice clouds events in three groups: Equatorial dawn, Equatorial dusk (both between 20°S and 20°N) and Southern midlatitudes at dawn (45°S and 55°S east of Hellas Basin) with ESA ExoMars Trace Gas Orbiter's Nadir and Occultation for MArs Discovery instrument. CO2ice abundance is retrieved simultaneously with water ice, dust, and particle sizes, and rotational temperature and CO2column profiles in 16 of 26 cases. Small particles (<0.5 μm) prevail at dusk, while water ice likely provides most source nuclei at dawn. Clouds east of Hellas are found to be dominantly nucleated on surface‐lifted dust. CO2ice is sometimes detected in unsaturated air together with dust nuclei at dawn, suggesting ongoing sublimation. Depending on latitude and local time, the interplay between particle precipitation and the lifetime of temperature minima (i.e., cold pockets) determines CO2ice properties. The upper atmosphere of Mars is characterized by the seasonal presence of CO2ice clouds. Their properties have been long studied, as well as their formation mechanisms in relation to the thermal structure of the atmosphere and its variability. In this study, we present the first observations of these clouds at the terminator (dawn and dusk) by the NOMAD spectrometer onboard the Exomars Trace Gas Orbiter. CO2ice is detected simultaneously with dust, water ice and the temperature profile. Our results agree with previous findings in terms of how clouds are spatially distributed and their temporal occurrence. However, we also explore the sources of condensation nuclei for CO2ice particles, showing that water ice is a possible source at dawn near the Equator. We also identify surface‐lifted dust below the CO2ice clouds observed east of Hellas Basin, suggesting that, at that location, dust could provide nuclei for CO2ice. CO2ice is also sometimes detected at temperatures higher than the CO2freezing point, suggesting ongoing sublimation. In this work we explore for the first time the composition of CO2ice clouds, which is critical to advance our understanding of how CO2ice clouds form in the mesosphere at Mars. Twenty Six mesospheric CO2ice clouds were detected with NOMAD SO in Mars Year 35, simultaneously with water ice, dust, and CO2saturation ratiosEquatorial CO2clouds are observed at 50–80 km altitude at dusk, and 40–60 km at dawn, when water ice likely provides condensation nucleiSix CO2ice clouds are found east of Hellas basin; their formation is likely sourced by surface‐lifted dust at 40–65 km Twenty Six mesospheric CO2ice clouds were detected with NOMAD SO in Mars Year 35, simultaneously with water ice, dust, and CO2saturation ratios Equatorial CO2clouds are observed at 50–80 km altitude at dusk, and 40–60 km at dawn, when water ice likely provides condensation nuclei Six CO2ice clouds are found east of Hellas basin; their formation is likely sourced by surface‐lifted dust at 40–65 km

Published
2021
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16. Probing the Atmospheric Cl Isotopic Ratio on Mars: Implications for Planetary Evolution and Atmospheric Chemistry

Author

Liuzzi, Giuliano, Villanueva, Geronimo L., Viscardy, Sebastien, Mège, Daniel, Crismani, Matteo M. J., Aoki, Shohei, Gurgurewicz, Joanna, Tesson, Pierre‐Antoine, Mumma, Michael J., Smith, Michael D., Faggi, Sara, Kofman, Vincent, Knutsen, Elise W., Daerden, Frank, Neary, Lori, Schmidt, Frédéric, Trompet, Loïc, Erwin, Justin T., Robert, Séverine, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Lopez‐Moreno, Jóse Juan, Patel, Manish R., Vandaele, Ann Carine, Liuzzi, Giuliano, Villanueva, Geronimo L., Viscardy, Sebastien, Mège, Daniel, Crismani, Matteo M. J., Aoki, Shohei, Gurgurewicz, Joanna, Tesson, Pierre‐Antoine, Mumma, Michael J., Smith, Michael D., Faggi, Sara, Kofman, Vincent, Knutsen, Elise W., Daerden, Frank, Neary, Lori, Schmidt, Frédéric, Trompet, Loïc, Erwin, Justin T., Robert, Séverine, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Lopez‐Moreno, Jóse Juan, Patel, Manish R., and Vandaele, Ann Carine

Abstract

Following the recent detection of HCl in the atmosphere of Mars by ExoMars/Trace Gas Orbiter, we present here the first measurement of the 37Cl/35Cl isotopic ratio in the Martian atmosphere using a set of Nadir Occultation for MArs Discovery (NOMAD) observations. We determine an isotopic anomaly of −6 ± 78‰ compared to Earth standard, consistent with the −51‰–−1‰ measured on Mars’ surface by Curiosity. The measured isotopic ratio is also consistent with surface measurements, and suggests that Cl reservoirs may have undergone limited processing since formation in the Solar Nebula. The examination of possible sources and sinks of HCl shows only limited pathways to short‐term efficient Cl fractionation and many plausible reservoirs of “light” Cl.

17. Water heavily fractionated as it ascends on Mars as revealed by ExoMars/NOMAD

Author

Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M. J., Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Smith, Michael D., Mumma, Michael J., Knutsen, Elise W., Neary, Lori, Viscardy, Sebastien, Thomas, Ian R., Lopez-Valverde, Miguel Angel, Ristic, Bojan, Patel, Manish R., Holmes, James A., Bellucci, Giancarlo, Lopez-Moreno, Jose Juan, Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M. J., Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Smith, Michael D., Mumma, Michael J., Knutsen, Elise W., Neary, Lori, Viscardy, Sebastien, Thomas, Ian R., Lopez-Valverde, Miguel Angel, Ristic, Bojan, Patel, Manish R., Holmes, James A., Bellucci, Giancarlo, and Lopez-Moreno, Jose Juan

Abstract

sotopic ratios and, in particular, the water D/H ratio are powerful tracers of the evolution and transport of water on Mars. From measurements performed with ExoMars/NOMAD, we observe marked and rapid variability of the D/H along altitude on Mars and across the whole planet. The observations (from April 2018 to April 2019) sample a broad range of events on Mars, including a global dust storm, the evolution of water released from the southern polar cap during southern summer, the equinox phases, and a short but intense regional dust storm. In three instances, we observe water at very high altitudes (>80 km), the prime region where water is photodissociated and starts its escape to space. Rayleigh distillation appears the be the driving force affecting the D/H in many cases, yet in some instances, the exchange of water reservoirs with distinctive D/H could be responsible.

18. Water heavily fractionated as it ascends on Mars as revealed by ExoMars/NOMAD

Author

Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M. J., Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Smith, Michael D., Mumma, Michael J., Knutsen, Elise W., Neary, Lori, Viscardy, Sebastien, Thomas, Ian R., Lopez-Valverde, Miguel Angel, Ristic, Bojan, Patel, Manish R., Holmes, James A., Bellucci, Giancarlo, Lopez-Moreno, Jose Juan, Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M. J., Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Smith, Michael D., Mumma, Michael J., Knutsen, Elise W., Neary, Lori, Viscardy, Sebastien, Thomas, Ian R., Lopez-Valverde, Miguel Angel, Ristic, Bojan, Patel, Manish R., Holmes, James A., Bellucci, Giancarlo, and Lopez-Moreno, Jose Juan

Abstract

sotopic ratios and, in particular, the water D/H ratio are powerful tracers of the evolution and transport of water on Mars. From measurements performed with ExoMars/NOMAD, we observe marked and rapid variability of the D/H along altitude on Mars and across the whole planet. The observations (from April 2018 to April 2019) sample a broad range of events on Mars, including a global dust storm, the evolution of water released from the southern polar cap during southern summer, the equinox phases, and a short but intense regional dust storm. In three instances, we observe water at very high altitudes (>80 km), the prime region where water is photodissociated and starts its escape to space. Rayleigh distillation appears the be the driving force affecting the D/H in many cases, yet in some instances, the exchange of water reservoirs with distinctive D/H could be responsible.

19. Water heavily fractionated as it ascends on Mars as revealed by ExoMars/NOMAD.

Author

Villanueva GL, Liuzzi G, Crismani MMJ, Aoki S, Vandaele AC, Daerden F, Smith MD, Mumma MJ, Knutsen EW, Neary L, Viscardy S, Thomas IR, Lopez-Valverde MA, Ristic B, Patel MR, Holmes JA, Bellucci G, and Lopez-Moreno JJ

Abstract

Isotopic ratios and, in particular, the water D/H ratio are powerful tracers of the evolution and transport of water on Mars. From measurements performed with ExoMars/NOMAD, we observe marked and rapid variability of the D/H along altitude on Mars and across the whole planet. The observations (from April 2018 to April 2019) sample a broad range of events on Mars, including a global dust storm, the evolution of water released from the southern polar cap during southern summer, the equinox phases, and a short but intense regional dust storm. In three instances, we observe water at very high altitudes (>80 km), the prime region where water is photodissociated and starts its escape to space. Rayleigh distillation appears the be the driving force affecting the D/H in many cases, yet in some instances, the exchange of water reservoirs with distinctive D/H could be responsible., (Copyright © 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. Distributed under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC).)

Published
2021
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