ExoMars TGO/NOMAD‐UVIS Vertical Profiles of Ozone: 2. The High‐Altitude Layers of Atmospheric Ozone. Issue 11 (18th November 2021)

• Record Type: Journal Article
• Authors: Khayat, Alain S. J.; Smith, Michael D.; Wolff, Michael; Daerden, Frank; Neary, Lori; Patel, Manish R.; Piccialli, Arianna; Vandaele, Ann C.; Thomas, Ian; Ristic, Bojan; Mason, Jon; Willame, Yannick; Depiesse, Cedric; Bellucci, Giancarlo; López‐Moreno, José Juan
• Is Part Of: Journal of geophysical research. Volume 126:Issue 11(2021)
• Page Start: n/a
• Page End: n/a
• Publication Date: 2021-11-18
• Subjects: Mars -- atmosphere -- composition -- ozone -- radiative transfer -- spacecraft; Planets -- Periodicals; Geophysics -- Periodicals; 559.9
• DOI: 10.1029/2021JE006834
• Languages: English
• ISSNs: 2169-9097

Abstract

Abstract: Solar occultations performed by the Nadir and Occultation for MArs Discovery (NOMAD) ultraviolet and visible spectrometer (UVIS) onboard the ExoMars Trace Gas Orbiter (TGO) have provided a comprehensive mapping of atmospheric ozone density. The observations here extend over a full Mars year (MY) between April 21, 2018 at the beginning of the TGO science operations during late northern summer on Mars (MY 34, L s = 163°) and March 9, 2020 (MY 35). UVIS provided transmittance spectra of the Martian atmosphere allowing measurements of the vertical distribution of ozone density using its Hartley absorption band (200–300 nm). The overall comparison to water vapor is found in the companion paper to this work (Patel et al., 2021, https://doi.org/10.1029/2021JE006837 ). Our findings indicate the presence of (a) a high‐altitude peak of ozone between 40 and 60 km in altitude over the north polar latitudes for at least 45% of the Martian year during midnorthern spring, late northern summer‐early southern spring, and late southern summer, and (b) a second, but more prominent, high‐altitude ozone peak in the south polar latitudes, lasting for at least 60% of the year including the southern autumn and winter seasons. When present, both high‐altitude peaks are observed in the sunrise and sunset occultations, suggesting that the layers could persist during the day. Results from the Mars general circulation models predict the general behavior of these peaks of ozone and are used in an attempt to further our understanding of the chemical processes controlling high‐altitude ozone on Mars. Plain Language Summary: The presence of ozone in the Martian atmosphere has been observed since it was first detected by the 1969 and 1971 Mariner flyby missions. Mars is known to have a permanent ozone layer below 30 km. Solar occultations performed by the ultraviolet and visible spectrometer onboard the ExoMars Trace Gas Orbiter have provided a comprehensive mapping of the vertical distribution of ozone in the atmosphere of Mars for an entire Mars year, describing the seasonal, spatial, and local time distribution of ozone in detail. This analysis indicates the presence of a previously undetected high‐altitude peak of ozone between 40 and 60 km in altitude over the north polar latitudes for approximately half of the Martian year. It also confirms the presence of a second, but more prominent, high‐altitude ozone peak in the south polar latitudes. When they are present, both high‐altitude peaks are observed in the sunrise and sunset occultations, indicating that the layers could persist during the day. Key Points: We provide the first detection of a high‐altitude peak of ozone between 40 and 60 km in altitude over the north polar latitudes of Mars We confirm the presence of a previously detected, more prominent high‐altitude ozone peak in the south polar latitudes Both high‐altitude peaks are observed in the sunrise and sunset occultations, indicating that the layers could persist during the day