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Water Vapor Vertical Distribution on Mars After Six Years of TGO/NOMAD Solar Occultations: 1. Global Climatology.

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Title: Water Vapor Vertical Distribution on Mars After Six Years of TGO/NOMAD Solar Occultations: 1. Global Climatology.
Authors: Brines, A.1 (AUTHOR) adrianbm@iaa.es, López‐Valverde, M. A.1 (AUTHOR), Funke, B.1 (AUTHOR), González‐Galindo, F.1 (AUTHOR), Aoki, S.2,3 (AUTHOR), Thomas, I. R.2 (AUTHOR), Villanueva, G. L.4 (AUTHOR), Liuzzi, G.5 (AUTHOR), Erwin, J. T.2 (AUTHOR), Grabowski, U.6 (AUTHOR), Forget, F.7 (AUTHOR), Lopez‐Moreno, J. J.1 (AUTHOR), Rodriguez‐Gomez, J.1 (AUTHOR), Daerden, F.2 (AUTHOR), Trompet, L.2 (AUTHOR), Ristic, B.2 (AUTHOR), Patel, M. R.8 (AUTHOR), Holmes, J. A.8 (AUTHOR), Bellucci, G.9 (AUTHOR), Modak, A.10 (AUTHOR)
Source: Journal of Geophysical Research. Planets. Feb2026, Vol. 131 Issue 2, p1-19. 19p.
Subject Terms: Water vapor, Martian atmosphere, Remote sensing of the atmosphere, Scientific apparatus & instruments, Seasonal physiological variations
Abstract: We present vertical profiles of water vapor obtained during six continuous years of solar occultation observations in the infrared by the Nadir and Occultation for MArs Discovery (NOMAD) instrument on board Trace Gas Orbiter. The retrievals have been performed with an inversion code previously applied to smaller samples of this data set, but improved to combine pairs of diffraction orders allowing for sounding water vapor up to about 120 km altitude. As a first part of a set of two papers, this study presents the most extended data set of water vapor measurements from the NOMAD instrument to date, covering three full and consecutive Martian Years. Building upon previous researches primarily focused on the perihelion season, this analysis now includes the aphelion season, offering a comprehensive view of Mars' water cycle. Observations from April 2018 to December 2023 were analyzed, covering perihelion of Mars Year (MY) 34 to aphelion of MY 37 and presenting water vapor vertical profiles from approximately 5–10 km to 110–120 km in altitude. This study reveals consistent seasonal and latitudinal water vapor patterns, showing water vapor systematically more vertically extended during the perihelion season than during the aphelion. We present an extensive analysis of the water vapor local time variability, confirming overall larger abundances during the evenings than during mornings. These data provide new insights into the vertical distribution of atmospheric water vapor on Mars, aiding future comparisons and global climate model validation. Plain Language Summary: Here we study water vapor in Mars' atmosphere, a key element for understanding the planet's climate and its evolution from a once warmer, wetter world to the cold, dry planet it is today. Although Mars currently has relatively small amounts of water vapor in the atmosphere, this vapor significantly influences surface and atmospheric processes, shaping the planet's complex water cycle. Using the Nadir and Occultation for MArs Discovery (NOMAD) instrument on the Trace Gas Orbiter, we analyzed infrared spectra taken from April 2018 to December 2023, spanning different seasons and times of day over three complete Martian years. We found that water vapor extends to higher altitudes during Mars' warmer season compared to the colder season. Additionally, water vapor was generally more abundant during the evenings than in the mornings. This work presents the most extensive data set on Mars' water vapor vertical distribution, providing a more comprehensive view of how water vapor varies across time and location on the planet. Key Points: Three complete Martian Years of water vapor vertical distribution from Mars' troposphere to mesopause using infrared solar occultationsMore vertically extended water vapor abundances during perihelion seasons compared to aphelion as a result of Mars' orbital eccentricityWater vapor morning enhancement at high altitudes in the northern hemisphere during the local winter [ABSTRACT FROM AUTHOR]
Copyright of Journal of Geophysical Research. Planets is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Water Vapor Vertical Distribution on Mars After Six Years of TGO/NOMAD Solar Occultations: 1. Global Climatology.
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Planets%22">Journal of Geophysical Research. Planets</searchLink>. Feb2026, Vol. 131 Issue 2, p1-19. 19p.
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  Data: We present vertical profiles of water vapor obtained during six continuous years of solar occultation observations in the infrared by the Nadir and Occultation for MArs Discovery (NOMAD) instrument on board Trace Gas Orbiter. The retrievals have been performed with an inversion code previously applied to smaller samples of this data set, but improved to combine pairs of diffraction orders allowing for sounding water vapor up to about 120 km altitude. As a first part of a set of two papers, this study presents the most extended data set of water vapor measurements from the NOMAD instrument to date, covering three full and consecutive Martian Years. Building upon previous researches primarily focused on the perihelion season, this analysis now includes the aphelion season, offering a comprehensive view of Mars' water cycle. Observations from April 2018 to December 2023 were analyzed, covering perihelion of Mars Year (MY) 34 to aphelion of MY 37 and presenting water vapor vertical profiles from approximately 5–10 km to 110–120 km in altitude. This study reveals consistent seasonal and latitudinal water vapor patterns, showing water vapor systematically more vertically extended during the perihelion season than during the aphelion. We present an extensive analysis of the water vapor local time variability, confirming overall larger abundances during the evenings than during mornings. These data provide new insights into the vertical distribution of atmospheric water vapor on Mars, aiding future comparisons and global climate model validation. Plain Language Summary: Here we study water vapor in Mars' atmosphere, a key element for understanding the planet's climate and its evolution from a once warmer, wetter world to the cold, dry planet it is today. Although Mars currently has relatively small amounts of water vapor in the atmosphere, this vapor significantly influences surface and atmospheric processes, shaping the planet's complex water cycle. Using the Nadir and Occultation for MArs Discovery (NOMAD) instrument on the Trace Gas Orbiter, we analyzed infrared spectra taken from April 2018 to December 2023, spanning different seasons and times of day over three complete Martian years. We found that water vapor extends to higher altitudes during Mars' warmer season compared to the colder season. Additionally, water vapor was generally more abundant during the evenings than in the mornings. This work presents the most extensive data set on Mars' water vapor vertical distribution, providing a more comprehensive view of how water vapor varies across time and location on the planet. Key Points: Three complete Martian Years of water vapor vertical distribution from Mars' troposphere to mesopause using infrared solar occultationsMore vertically extended water vapor abundances during perihelion seasons compared to aphelion as a result of Mars' orbital eccentricityWater vapor morning enhancement at high altitudes in the northern hemisphere during the local winter [ABSTRACT FROM AUTHOR]
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  Data: <i>Copyright of Journal of Geophysical Research. Planets is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
PLink https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&db=8gh&AN=191834821
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