Explaining NOMAD D/H Observations by Cloud‐Induced Fractionation of Water Vapor on Mars

Daerden, Frank; Neary, L.; Villanueva, Gerónimo; Liuzzi, Giuliano; Aoki, Shohei; Clancy, R. T.; Whiteway, J.; Sandor, Brad J.; Smith, M. D.; Wolff, Michael; Pankine, A.; Khayat, Alain; Novak, R. E.; Cantor, B. A.; Crismani, Matteo; Mumma, M. J.; Viscardy, S.; Erwin, Justin; Depiesse, C.; Mahieux, A.; Piccialli, Arianna; Robert, Séverine; Trompet, Loïc; Willame, Yannick; Neefs, Eddy; Thomas, Ian; Ristic, Bojan; Vandaele, Ann Carine

doi:10.1029/2021je007079

Cited by 13 publications

(43 citation statements)

References 83 publications

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“…This is consistent with our initial reports in Villanueva et al. (2021) and GCM modeling (Daerden et al., 2022; Rossi et al., 2021), as well as complementary measurements with the ACS spectrometer suite (Alday, Trokhimovskiy, et al., 2021), which highlights the strong variability of this parameter with altitude. Alday, Trokhimovskiy, et al.…”

Section: The Seasonal and Spatial Variability Of The D/hsupporting

confidence: 92%

“…In all cases (all seasons and regions of the planet), the D/H declines quickly above the hygropause, from a nominal value above 5 VSMOW to a very low value near <2 VSMOW when HDO is not present (owing to its preferential freeze-out). This is consistent with our initial reports in Villanueva et al (2021) and GCM modeling (Daerden et al, 2022;Rossi et al, 2021), as well as complementary measurements with the ACS spectrometer suite , which highlights the strong variability of this parameter with altitude. reports a D/H greater than 5-6 VSMOW during southern summer (L S ∼ 190°-300°) in the 10-60 km altitude range, consistent within error-bars (1 VSMOW) with our findings as reported in Figure 1, which show red colors (∼6 VSMOW) for this season/altitude.…”

Section: The Seasonal and Spatial Variability Of The D/hsupporting

confidence: 92%

“…Our previous ground-based observations of the total water column (Villanueva et al, 2015), at L S ∼ 80° and primarily weighted to the lower part of the hygropause, indicate a typical D/H of ∼7 VSMOW for the Northern Hemisphere seasonal release. Assuming as reference the other seasons as shown in Figure 2 and complementary isotopic fractionation modeling (Daerden et al, 2022), a value of ∼5-7 VSMOW close to the hygropause as reported here is consistent with the previous ground-based observations. Importantly, this would mean that the D/H of the water liberated from the seasonal northern polar cap is the same as that of the water liberated from the seasonal southern polar cap, roughly 6-7 VSMOW.…”

Section: The Seasonal and Spatial Variability Of The D/hsupporting

confidence: 91%

“…This was already anticipated from cloud detections in northern summer by the Phoenix mission (Whiteway et al, 2009) and their simulated impact on the vertical distribution of water vapor (Daerden et al, 2010). (Note: GCM simulations shown in Daerden et al (2022) do not sufficiently confine water vapor so low due to a simplistic cloud description.). In all cases (all seasons and regions of the planet), the D/H declines quickly above the hygropause, from a nominal value above 5 VSMOW to a very low value near <2 VSMOW when HDO is not present (owing to its preferential freeze-out).…”

Section: The Seasonal and Spatial Variability Of The D/hmentioning

confidence: 78%

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The Deuterium Isotopic Ratio of Water Released From the Martian Caps as Measured With TGO/NOMAD

Villanueva

Liuzzi

Aoki

et al. 2022

Geophysical Research Letters

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The evolution and history of water on Mars plays a key role in the assessment of the habitability of the planet across time. There is abundant geomorphological evidence suggesting that Mars had a wetter past (Bibring et al., 2006;Carr & Head, 2003), yet the duration and extent of this more humid past remains a topic of substantial debate. For instance, the large deltas, basins, and valleys on Mars are suggestive of large bodies of water that were stable over relatively long periods of time. Some estimates suggest past volumes of water in excess of a 500 m deep Global Equivalent Layer (GEL; Carr & Head, 2003), which is many times larger than the current estimates of labile water on Mars (∼30 m, Lasue et al., 2013).The large enrichments of D/H measured in atmospheric water suggest that a large fraction, beyond 80%, of this water was lost over time (Jakosky, 2021;Villanueva et al., 2015), and Ar and O isotopic ratios measured with MAVEN (Jakosky et al., 2017) and TGO (Alday, Wilson, et al., 2021) indicate that Mars has lost a large fraction of its atmosphere. Because Mars is less massive than Earth, the neutral escape of volatiles is easier on Mars, considering the similar equilibrium temperatures of the two planets, although Mars is obviously colder. Recent results indicate that most of this escape occurred via neutral and nonionized processes (Brain et al., 2015), in which temperature and its variability across geological times were key factors defining the state of the Martian atmosphere. Recent results from dust storms suggest that dust storms can greatly heat the atmosphere, leading to the upward transport and more readily escape of water (

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Section: The Seasonal and Spatial Variability Of The D/hsupporting

confidence: 92%

Section: The Seasonal and Spatial Variability Of The D/hsupporting

confidence: 92%

Section: The Seasonal and Spatial Variability Of The D/hsupporting

confidence: 91%

Section: The Seasonal and Spatial Variability Of The D/hmentioning

confidence: 78%

See 2 more Smart Citations

The Deuterium Isotopic Ratio of Water Released From the Martian Caps as Measured With TGO/NOMAD

Villanueva

Liuzzi

Aoki

et al. 2022

Geophysical Research Letters

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“…Both of these facets are particularly helpful for the lower transmittances found in dusty conditions, and so to provide a clearer picture in the 2018 GDS. We will also investigate the behavior of odd hydrogen and odd oxygen (including O 3 ) using a GCM that is operated for the conditions of Martian years (MY) 34 and 35 (Daerden et al., 2022; Neary et al., 2020) and that includes detailed atmospheric chemistry routines (Daerden et al., 2019). Combining the filtered observations with the model simulations then allows to obtain a detailed picture of the changes in atmospheric chemistry during the 2018 GDS.…”

Section: Introductionmentioning

confidence: 99%

Planet‐Wide Ozone Destruction in the Middle Atmosphere on Mars During Global Dust Storm

Daerden

Neary

Wolff

et al. 2022

Geophysical Research Letters

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The Nadir and Occultation for MArs Discovery (NOMAD)/UV‐visible (UVIS) spectrometer on the ExoMars Trace Gas Orbiter provided observations of ozone (O3) and water vapor in the global dust storm of 2018. Here we show in detail, using advanced data filtering and chemical modeling, how Martian O3 in the middle atmosphere was destroyed during the dust storm. In data taken exactly 1 year later when no dust storm occurred, the normal situation had been reestablished. The model simulates how water vapor is transported to high altitudes and latitudes in the storm, where it photolyzes to form odd hydrogen species that catalyze O3. O3 destruction is simulated at all latitudes and up to 100 km, except near the surface where it increases. The simulations also predict a strong increase in the photochemical production of atomic hydrogen in the middle atmosphere, consistent with the enhanced hydrogen escape observed in the upper atmosphere during global dust storms.

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Martian Ozone Observed by TGO/NOMAD‐UVIS Solar Occultation: An Inter‐Comparison of Three Retrieval Methods

Piccialli

Vandaele

Willame

et al. 2023

Earth and Space Science

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The NOMAD‐UVIS instrument on board the ExoMars Trace Gas Orbiter has been investigating the Martian atmosphere with the occultation technique since April 2018. Here, we analyze almost two Mars Years of ozone vertical distributions acquired at the day‐night terminator. The ozone retrievals proved more difficult than expected due to spurious detections of ozone caused by instrumental effects, high dust content, and very low values of ozone. This led us to compare the results from three different retrieval approaches: (a) an onion peeling method, (b) a full occultation Optimal Estimation Method, and (c) a direct onion peeling method. The three methods produce consistently similar results, especially where ozone densities are higher. The main challenge was to find reliable criteria to exclude spurious detections of O3, and we finally adopted two criteria for filtering: (a) a detection limit, and (b) the Δχ2 criterion. Both criteria exclude spurious O3 values especially near the perihelion (180° < Ls < 340°), where up to 98% of ozone detections are filtered out, in agreement with general circulation models, that expect very low values of ozone in this season. Our agrees well with published analysis of the NOMAD‐UVIS data set, as we confirm the main features observed previously, that is, the high‐altitude ozone peak around 40 km at high latitudes. The filtering approaches are in good agreement with those implemented for the SPICAM/MEx observations and underline the need to evaluate carefully the quality of ozone retrievals in occultations.

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Explaining NOMAD D/H Observations by Cloud‐Induced Fractionation of Water Vapor on Mars

Abstract: The heavy water isotope, D 2 O, is several orders of magnitude less abundant.) Also on Mars, it is expected that the HDO/H 2 O isotopic ratio is an important marker for atmospheric water vapor

Cited by 13 publications

References 83 publications

The Deuterium Isotopic Ratio of Water Released From the Martian Caps as Measured With TGO/NOMAD

The Deuterium Isotopic Ratio of Water Released From the Martian Caps as Measured With TGO/NOMAD

Planet‐Wide Ozone Destruction in the Middle Atmosphere on Mars During Global Dust Storm

Martian Ozone Observed by TGO/NOMAD‐UVIS Solar Occultation: An Inter‐Comparison of Three Retrieval Methods

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