Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV
Cross-hemispheric circulation of the atmosphere is a major feature of the Martian troposphere and Venusian thermosphere. On Mars, it is driven by the latitudinal gradient of insolation at the surface, which generates a global summer-to-winter Hadley cell reversing orientation during equinoxes and ma...
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ftuniversailles:oai:HAL:hal-00667054v1 2023-07-30T04:06:28+02:00 Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV Montmessin, Franck Bertaux, Jean-Loup Lefèvre, Franck Gondet, Brigitte Marcq, Emmanuel Reberac, Aurélie Sarago, Vincent PLANETO - LATMOS Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS) Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS) Institut d'astrophysique spatiale (IAS) Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales Paris (CNES) Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS) Pasadena, United States 2010-10 https://hal.science/hal-00667054 en eng HAL CCSD hal-00667054 https://hal.science/hal-00667054 BIBCODE: 2010DPS.42.4206M 42nd Annual Meeting of the Division for Planetary Sciences (DPS) https://hal.science/hal-00667054 42nd Annual Meeting of the Division for Planetary Sciences (DPS), Oct 2010, Pasadena, United States [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] info:eu-repo/semantics/conferenceObject Conference papers 2010 ftuniversailles 2023-07-16T20:14:39Z Cross-hemispheric circulation of the atmosphere is a major feature of the Martian troposphere and Venusian thermosphere. On Mars, it is driven by the latitudinal gradient of insolation at the surface, which generates a global summer-to-winter Hadley cell reversing orientation during equinoxes and maximizing intensity at solstices. On Venus, it is driven by a longitudinal gradient between the dayside and the nightside and takes place above the super-rotating mesosphere and troposphere. This subsolar-to-antisolar (SSAS) circulation is known to induce major observational features, such as the vast O2 and NO emission zones observed close to midnight. Recently, SPICAV onboard Venus Express has detected for the first time the presence of ozone on Venus, accounting for a thin thermospheric layer at about 100 km. We suggest that this ozone layer forms as a result of O atoms carried from the dayside and recombining in the subsiding branch of the SSAS where the O2 singlet delta emission is also observed. Interestingly, a similar feature was recently identified on Mars with SPICAM, with the presence of a >10 km thick ozone layer in the southern winter hemisphere near the pole. Contrarily to the ozone layer otherwise observed on Mars which extends from the surface and is controlled by reaction with HOx radicals, this layer is only related to O atoms produced in the summer hemisphere and carried via global circulation towards the polar night where they can recombine, yielding the newly detected O2 emission feature evidenced by OMEGA. Conference Object polar night Université de Versailles Saint-Quentin-en-Yvelines: HAL-UVSQ Venus ENVELOPE(-57.842,-57.842,-61.925,-61.925) |
institution |
Open Polar |
collection |
Université de Versailles Saint-Quentin-en-Yvelines: HAL-UVSQ |
op_collection_id |
ftuniversailles |
language |
English |
topic |
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] |
spellingShingle |
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] Montmessin, Franck Bertaux, Jean-Loup Lefèvre, Franck Gondet, Brigitte Marcq, Emmanuel Reberac, Aurélie Sarago, Vincent Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV |
topic_facet |
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] |
description |
Cross-hemispheric circulation of the atmosphere is a major feature of the Martian troposphere and Venusian thermosphere. On Mars, it is driven by the latitudinal gradient of insolation at the surface, which generates a global summer-to-winter Hadley cell reversing orientation during equinoxes and maximizing intensity at solstices. On Venus, it is driven by a longitudinal gradient between the dayside and the nightside and takes place above the super-rotating mesosphere and troposphere. This subsolar-to-antisolar (SSAS) circulation is known to induce major observational features, such as the vast O2 and NO emission zones observed close to midnight. Recently, SPICAV onboard Venus Express has detected for the first time the presence of ozone on Venus, accounting for a thin thermospheric layer at about 100 km. We suggest that this ozone layer forms as a result of O atoms carried from the dayside and recombining in the subsiding branch of the SSAS where the O2 singlet delta emission is also observed. Interestingly, a similar feature was recently identified on Mars with SPICAM, with the presence of a >10 km thick ozone layer in the southern winter hemisphere near the pole. Contrarily to the ozone layer otherwise observed on Mars which extends from the surface and is controlled by reaction with HOx radicals, this layer is only related to O atoms produced in the summer hemisphere and carried via global circulation towards the polar night where they can recombine, yielding the newly detected O2 emission feature evidenced by OMEGA. |
author2 |
PLANETO - LATMOS Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS) Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS) Institut d'astrophysique spatiale (IAS) Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales Paris (CNES) Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS) |
format |
Conference Object |
author |
Montmessin, Franck Bertaux, Jean-Loup Lefèvre, Franck Gondet, Brigitte Marcq, Emmanuel Reberac, Aurélie Sarago, Vincent |
author_facet |
Montmessin, Franck Bertaux, Jean-Loup Lefèvre, Franck Gondet, Brigitte Marcq, Emmanuel Reberac, Aurélie Sarago, Vincent |
author_sort |
Montmessin, Franck |
title |
Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV |
title_short |
Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV |
title_full |
Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV |
title_fullStr |
Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV |
title_full_unstemmed |
Transport-driven formation of an ozone layer on Venus and Mars as evidenced by SPICAM and SPICAV |
title_sort |
transport-driven formation of an ozone layer on venus and mars as evidenced by spicam and spicav |
publisher |
HAL CCSD |
publishDate |
2010 |
url |
https://hal.science/hal-00667054 |
op_coverage |
Pasadena, United States |
long_lat |
ENVELOPE(-57.842,-57.842,-61.925,-61.925) |
geographic |
Venus |
geographic_facet |
Venus |
genre |
polar night |
genre_facet |
polar night |
op_source |
42nd Annual Meeting of the Division for Planetary Sciences (DPS) https://hal.science/hal-00667054 42nd Annual Meeting of the Division for Planetary Sciences (DPS), Oct 2010, Pasadena, United States |
op_relation |
hal-00667054 https://hal.science/hal-00667054 BIBCODE: 2010DPS.42.4206M |
_version_ |
1772819076922474496 |