Seasonal variation of ozone vertical profiles form ExoMars TGO and comparison to water

Manish R. Patel; Graham Seller; Jonathon Mason; James Holmes; Megan Brown; Stephen Lewis; Kylash Rajendran; Paul Streeter; Charlotte Marriner; Brijen Hathi; David Slade; Mark Leese; Mike Wolff; Alain Khayat; Michael Smith; Shohei Aoki; Arianna Piccialli; Ann Carine Vandaele; Severine Robert; Frank Daerden

doi:https://doi.org/10.5194/epsc2021-550

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EPSC Abstracts

Vol. 15, EPSC2021-550, 2021, updated on 09 Jan 2024

https://doi.org/10.5194/epsc2021-550

Europlanet Science Congress 2021

© Author(s) 2024. This work is distributed under
the Creative Commons Attribution 4.0 License.

Seasonal variation of ozone vertical profiles form ExoMars TGO and comparison to water

Manish R. Patel^1,2, Graham Seller¹, Jonathon Mason¹, James Holmes¹, Megan Brown¹, Stephen Lewis¹, Kylash Rajendran¹, Paul Streeter¹, Charlotte Marriner¹, Brijen Hathi¹, David Slade¹, Mark Leese¹, Mike Wolff³, Alain Khayat⁴, Michael Smith⁴, Shohei Aoki⁵, Arianna Piccialli⁵, Ann Carine Vandaele⁵, Severine Robert⁵, Frank Daerden⁵, and the the NOMAD Team^*

Manish R. Patel et al.

¹The Open University, Milton Keynes, U.K. (manish.patel@open.ac.uk)
²Space Science and Technology Department, Science and Technology Facilities Council, Rutherford Appleton Laboratory, Oxfordshire, U.K
³Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, UCB 564, USA.
⁴NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
⁵Royal Belgian Institute for Space Aeronomy, BIRA-IASB, 3 Avenue Circulaire, 1180 Brussels, Belgium.
^*A full list of authors appears at the end of the abstract

The Ultraviolet and Visible Spectrometer (UVIS) channel [1] of the Nadir and Occultation for Mars Discovery (NOMAD) instrument [2] aboard the ExoMars Trace Gas Orbiter has been making observations of the vertical, latitudinal and seasonal distributions of ozone. Here, we present ~1.5 Mars Years (MY) of vertical profiles of ozone, from L_S = 163° in MY34 to L_S = 320° in MY35. This period includes the occurrence of the MY34 Global Dust Storm. The relative abundance of both ozone and water (from coincident NOMAD measurements) increases with decreasing altitude below ~40 km at perihelion and at aphelion, localised decreases in ozone abundance exist between 25-35 km coincident with the location of modelled peak water abundances. High latitude (> ± 55°), high altitude (40-55 km) equinoctial ozone enhancements are observed in both hemispheres (L_S ~350‑40°). Morning terminator observations show elevated ozone abundances with respect to evening observations, most likely attributed to diurnal photochemical partitioning along the line of sight between ozone and O. The ozone retrievals presented here provide the most complete global description of Mars ozone vertical distributions to date as a function of season and latitude

the NOMAD Team:

Ian Thomas Bojan Ristic Yannick Willame Cedric Depiesse Giancarlo Bellucci Jose Lopez-Moreno

How to cite: Patel, M. R., Seller, G., Mason, J., Holmes, J., Brown, M., Lewis, S., Rajendran, K., Streeter, P., Marriner, C., Hathi, B., Slade, D., Leese, M., Wolff, M., Khayat, A., Smith, M., Aoki, S., Piccialli, A., Vandaele, A. C., Robert, S., and Daerden, F. and the the NOMAD Team: Seasonal variation of ozone vertical profiles form ExoMars TGO and comparison to water, Europlanet Science Congress 2021, online, 13–24 Sep 2021, EPSC2021-550, https://doi.org/10.5194/epsc2021-550, 2021.