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Martian dust and water cycle interactions inferred from NOMAD observations and semi-interactive GCM simulations

Presentation #318.01 in the session Mars’s Story as Told and Influenced by Dust and Water (Oral Presentation)

Published onOct 23, 2023
Martian dust and water cycle interactions inferred from NOMAD observations and semi-interactive GCM simulations

We present the dust-water cycle transport during major dust storms, using general circulation simulations (GCM) together with orbiter observations. The model was already used to investigate the Martian turbulence-dust feedback mechanisms between Mars Years 24-34 that exhibited three planet-encircling dust storms [1]. The dust scheme in the GCM was an in-house semi-interactive dust transport model [1] built in the MarsWRF [2], as governed by column dust climatology observations [3]. The model, however, used the water cycle in the MarsWRF that assumes simplified microphysics with monodisperse water ice particles. By combining the size-aware two-moment water cycle microphysics model of Lee et al. (2021) [4] with our semi-interactive dust transport model [1], we updated the dust-water cycle. Here we present the updated GCM simulations for Mars Years 34-36 in comparison with observations from Nadir and Occultation for Mars Discovery (NOMAD) instrument onboard the ExoMars Trace Gas Orbiter (TGO) [5]. Vandaele et al. (2019) [5] explored a rapid and large enhancement of the water vapor in the middle atmosphere driven by Martian major dust storms. Nomad observations revealed water vapor expansion to high altitudes up to 100 km during major dust storm episodes [6]. Additionally, Neary et al. (2020) [7] have shown that the size of the water ice particles controls the intensity of the cloud radiative feedback, which influences both the temperature and the water vapor profiles. The middle-upper atmospheric interactions are important as rapid dust tides transported meridionally may contribute to the water enhancement and hydrogen escape at the upper atmosphere [8].

[1] Senel et al. (2021). JGR: Planets, 126(10), e2021JE006965.

[2] Richardson et al. (2007). JGR: Planets, 112(E9).

[3] Montabone et al. (2020). JGR: Planets, 125(8), e2019JE006111.

[4] Lee et al. (2018). Icarus, 311, 23-34.

[5] Vandaele et al. (2019). Nature, 568(7753), 521-525.

[6] Aoki et al. (2019). JGR: Planets, 124(12), 3482-3497.

[7] Neary et al. (2020).Geophysical ResearchLetters, 47, e2019GL084354.

[8] Wu et al. (2020). Nature Communications, 11(1), 614.

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