The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter
Carbon monoxide (CO) is the main product of CO2 photolysis in the Martian atmosphere. Production of CO is balanced by its loss reaction with OH, which recycles CO into CO2. CO is therefore a sensitive tracer of the OH-catalysed chemistry that contributes to the stability of CO2 in the atmosphere of...
| Main Authors: | , , , , , , , , , , , , , |
|---|---|
| Format: | Journal article |
| Language: | English |
| Published: |
Springer Nature
2021
|
| _version_ | 1797097568667172864 |
|---|---|
| author | Olsen, KS Lefevre, F Montmessin, F Fedorova, AA Trokhimovskiy, A Baggio, L Korablev, O Alday, J Wilson, CF Forget, F Belyaev, DA Patrakeev, A Grigoriev, AV Shakun, A |
| author_facet | Olsen, KS Lefevre, F Montmessin, F Fedorova, AA Trokhimovskiy, A Baggio, L Korablev, O Alday, J Wilson, CF Forget, F Belyaev, DA Patrakeev, A Grigoriev, AV Shakun, A |
| author_sort | Olsen, KS |
| collection | OXFORD |
| description | Carbon monoxide (CO) is the main product of CO2 photolysis in the Martian atmosphere. Production of CO is balanced by its loss reaction with OH, which recycles CO into CO2. CO is therefore a sensitive tracer of the OH-catalysed chemistry that contributes to the stability of CO2 in the atmosphere of Mars. To date, CO has been measured only in terms of vertically integrated column abundances, and the upper atmosphere, where CO is produced, is largely unconstrained by observations. Here we report vertical profiles of CO from 10 to 120 km, and from a broad range of latitudes, inferred from the Atmospheric Chemistry Suite on board the ExoMars Trace Gas Orbiter. At solar longitudes 164–190°, we observe an equatorial CO mixing ratio of ~1,000 ppmv (10–80 km), increasing towards the polar regions to more than 3,000 ppmv under the influence of downward transport of CO from the upper atmosphere, providing a view of the Hadley cell circulation at Mars’s equinox. Observations also cover the 2018 global dust storm, during which we observe a prominent depletion in the CO mixing ratio up to 100 km. This is indicative of increased CO oxidation in a context of unusually large high-altitude water vapour, boosting OH abundance. |
| first_indexed | 2024-03-07T04:57:25Z |
| format | Journal article |
| id | oxford-uuid:d713f276-a924-4d57-9daa-4181210cad81 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T04:57:25Z |
| publishDate | 2021 |
| publisher | Springer Nature |
| record_format | dspace |
| spelling | oxford-uuid:d713f276-a924-4d57-9daa-4181210cad812022-03-27T08:38:27ZThe vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas OrbiterJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:d713f276-a924-4d57-9daa-4181210cad81EnglishSymplectic ElementsSpringer Nature2021Olsen, KSLefevre, FMontmessin, FFedorova, AATrokhimovskiy, ABaggio, LKorablev, OAlday, JWilson, CFForget, FBelyaev, DAPatrakeev, AGrigoriev, AVShakun, ACarbon monoxide (CO) is the main product of CO2 photolysis in the Martian atmosphere. Production of CO is balanced by its loss reaction with OH, which recycles CO into CO2. CO is therefore a sensitive tracer of the OH-catalysed chemistry that contributes to the stability of CO2 in the atmosphere of Mars. To date, CO has been measured only in terms of vertically integrated column abundances, and the upper atmosphere, where CO is produced, is largely unconstrained by observations. Here we report vertical profiles of CO from 10 to 120 km, and from a broad range of latitudes, inferred from the Atmospheric Chemistry Suite on board the ExoMars Trace Gas Orbiter. At solar longitudes 164–190°, we observe an equatorial CO mixing ratio of ~1,000 ppmv (10–80 km), increasing towards the polar regions to more than 3,000 ppmv under the influence of downward transport of CO from the upper atmosphere, providing a view of the Hadley cell circulation at Mars’s equinox. Observations also cover the 2018 global dust storm, during which we observe a prominent depletion in the CO mixing ratio up to 100 km. This is indicative of increased CO oxidation in a context of unusually large high-altitude water vapour, boosting OH abundance. |
| spellingShingle | Olsen, KS Lefevre, F Montmessin, F Fedorova, AA Trokhimovskiy, A Baggio, L Korablev, O Alday, J Wilson, CF Forget, F Belyaev, DA Patrakeev, A Grigoriev, AV Shakun, A The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter |
| title | The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter |
| title_full | The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter |
| title_fullStr | The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter |
| title_full_unstemmed | The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter |
| title_short | The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter |
| title_sort | vertical structure of co in the martian atmosphere from the exomars trace gas orbiter |
| work_keys_str_mv | AT olsenks theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT lefevref theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT montmessinf theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT fedorovaaa theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT trokhimovskiya theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT baggiol theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT korablevo theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT aldayj theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT wilsoncf theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT forgetf theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT belyaevda theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT patrakeeva theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT grigorievav theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT shakuna theverticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT olsenks verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT lefevref verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT montmessinf verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT fedorovaaa verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT trokhimovskiya verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT baggiol verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT korablevo verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT aldayj verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT wilsoncf verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT forgetf verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT belyaevda verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT patrakeeva verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT grigorievav verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter AT shakuna verticalstructureofcointhemartianatmospherefromtheexomarstracegasorbiter |