• Login
     
    View Item 
    •   ORFEO Home
    • Royal Belgian Institute for Space Aeronomy
    • BIRA-IASB publications
    • View Item
    •   ORFEO Home
    • Royal Belgian Institute for Space Aeronomy
    • BIRA-IASB publications
    • View Item
    JavaScript is disabled for your browser. Some features of this site may not work without it.

    Water Vapor Vertical Distribution on Mars During Perihelion Season of MY 34 and MY 35 With ExoMars-TGO/NOMAD Observations

    Thumbnail
    View/Open
    Brines(2023a).pdf (19.49Mb)
    Authors
    Brines, A.
    López-Valverde, M.A.
    Stolzenbach, A.
    Modak, A.
    Funke, B.
    Galindo, F.G.
    Aoki, S.
    Villanueva, G.L.
    Liuzzi, G.
    Thomas, I.R.
    Erwin, J.T.
    Grabowski, U.
    Forget, F.
    Lopez-Moreno, J.J.
    Rodriguez-Gomez, J.
    Daerden, F.
    Trompet, L.
    Ristic, B.
    Patel, M.R.
    Bellucci, G.
    Vandaele, A.C.
    Show allShow less
    Discipline
    Physical sciences
    Subject
    ExoMars
    TGO/NOMAD
    water vapor
    Audience
    Scientific
    Date
    2023
    Metadata
    Show full item record
    Description
    The water vapor in the Martian atmosphere plays a significant role in the planet's climate, being crucial in most of the chemical and radiative transfer processes. Despite its importance, the vertical distribution of H2O in the atmosphere has not still been characterized precisely enough. The recent ExoMars Trace Gas Orbiter mission, with its Nadir and Occultation for MArs Discovery instrument, has allowed us to measure the H2O vertical distribution with unprecedented resolution. Recent studies of vertical profiles have shown that high dust concentration in the atmosphere, in particular during dust storms, induces an efficient transport of the H2O to higher altitudes, from 40 km up to 80 km. We study the H2O vertical distribution in a subset of solar occultations during the perihelion of two Martian years (MYs), including the 2018 Global Dust Storm (GDS), in order to compare the same Martian season under GDS and non-GDS conditions. We present our state-of-the-art retrieval scheme, and we apply it to a combination of two diffraction orders, which permits sounding up to about 100 km. We confirm recent findings of H2O increasing at high altitudes during Ls = 190°–205° in MY 34, reaching abundances of about 150 ppmv at 80 km in both hemispheres not found during the same period of MY 35. We found a hygropause's steep rising during the GDS from 30 up to 80 km. Furthermore, strong supersaturation events have been identified at mesospheric altitudes even in presence of water ice layers retrieved by the IAA team.
    Citation
    Brines, A.; López-Valverde, M.A.; Stolzenbach, A.; Modak, A.; Funke, B.; Galindo, F.G.; Aoki, S.; Villanueva, G.L.; Liuzzi, G.; Thomas, I.R.; Erwin, J.T.; Grabowski, U.; Forget, F.; Lopez-Moreno, J.J.; Rodriguez-Gomez, J.; Daerden, F.; Trompet, L.; Ristic, B.; Patel, M.R.; Bellucci, G.; Vandaele, A.C. (2023). Water Vapor Vertical Distribution on Mars During Perihelion Season of MY 34 and MY 35 With ExoMars-TGO/NOMAD Observations. , Journal of Geophysical Research: Planets, Vol. 128, Issue 11, e2022JE007273, DOI: 10.1029/2022JE007273.
    Identifiers
    uri: https://orfeo.belnet.be/handle/internal/11170
    doi: http://dx.doi.org/10.1029/2022JE007273
    url:
    Type
    Article
    Peer-Review
    Yes
    Language
    eng
    Links
    NewsHelpdeskBELSPO OA Policy

    Browse

    All of ORFEOCommunities & CollectionsBy Issue DateAuthorsTitlesDisciplinesThis CollectionBy Issue DateAuthorsTitlesDisciplines
     

    DSpace software copyright © 2002-2016  DuraSpace
    Send Feedback | Cookie Information
    Theme by 
    Atmire NV