The CH4 abundance in Jupiter’s upper atmosphere

Hydrocarbon species, and in particular CH4, play a key role in the stratosphere-thermosphere boundary of Jupiter, which occurs around the μ-bar pressure level. Previous analyses of solar occultation, He and Ly-α airglow, and ISO/SWS measurements of the radiance around 3.3 μm have inferred significan...

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Detalhes bibliográficos
Autores: Sánchez-López, A., López-Puertas, Manuel, García Comas, Maia, Funke, Bernd, Fouchet, T., Snellen, I. A. G.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/285726
Acesso em linha:http://hdl.handle.net/10261/285726
Access Level:acceso abierto
Palavra-chave:Planets and satellites: atmospheres
Methods: data analysis - techniques: spectroscopic
Planets and satellites: individual: Jupiter
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spelling The CH4 abundance in Jupiter’s upper atmosphereSánchez-López, A.López-Puertas, ManuelGarcía Comas, MaiaFunke, BerndFouchet, T.Snellen, I. A. G.Planets and satellites: atmospheresMethods: data analysis - techniques: spectroscopicPlanets and satellites: individual: JupiterHydrocarbon species, and in particular CH4, play a key role in the stratosphere-thermosphere boundary of Jupiter, which occurs around the μ-bar pressure level. Previous analyses of solar occultation, He and Ly-α airglow, and ISO/SWS measurements of the radiance around 3.3 μm have inferred significantly different methane concentrations. Here we aim to accurately model the CH4 radiance at 3.3 μm measured by ISO/SWS by using a comprehensive non-local thermodynamic equilibrium model and the most recent collisional rates measured in the laboratory for CH4 to shed new light onto the methane concentration in the upper atmosphere of Jupiter. These emission bands have been shown to present a peak contribution precisely at the μ-bar level, hence directly probing the region of interest. We find that a high CH4 concentration is necessary to explain the data, in contrast with the most recent analyses, and that the observations favour the lower limit of the latest laboratory measurements of the CH4 collisional relaxation rates. Our results provide precise constraints on the composition and dynamics of the lower atmosphere of Jupiter. © ESO 2022.A.S.L. and I.S. acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program under grant agreement No 694513. IAA-CSIC authors acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades through projects Ref. PID2019-110689RB-I00/AEI/10.13039/501100011033 and the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709).Peer reviewedEDP SciencesMinisterio de Ciencia e Innovación (España)European CommissionEuropean Research CouncilConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202220222022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/285726reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//SEV-2017-0709info:eu-repo/grantAgreement/EC/H2020/694513info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-110689RB-I00http://dx.doi.org/10.1051/0004-6361/202141933Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2857262026-05-22T06:33:51Z
dc.title.none.fl_str_mv The CH4 abundance in Jupiter’s upper atmosphere
title The CH4 abundance in Jupiter’s upper atmosphere
spellingShingle The CH4 abundance in Jupiter’s upper atmosphere
Sánchez-López, A.
Planets and satellites: atmospheres
Methods: data analysis - techniques: spectroscopic
Planets and satellites: individual: Jupiter
title_short The CH4 abundance in Jupiter’s upper atmosphere
title_full The CH4 abundance in Jupiter’s upper atmosphere
title_fullStr The CH4 abundance in Jupiter’s upper atmosphere
title_full_unstemmed The CH4 abundance in Jupiter’s upper atmosphere
title_sort The CH4 abundance in Jupiter’s upper atmosphere
dc.creator.none.fl_str_mv Sánchez-López, A.
López-Puertas, Manuel
García Comas, Maia
Funke, Bernd
Fouchet, T.
Snellen, I. A. G.
author Sánchez-López, A.
author_facet Sánchez-López, A.
López-Puertas, Manuel
García Comas, Maia
Funke, Bernd
Fouchet, T.
Snellen, I. A. G.
author_role author
author2 López-Puertas, Manuel
García Comas, Maia
Funke, Bernd
Fouchet, T.
Snellen, I. A. G.
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
European Commission
European Research Council
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Planets and satellites: atmospheres
Methods: data analysis - techniques: spectroscopic
Planets and satellites: individual: Jupiter
topic Planets and satellites: atmospheres
Methods: data analysis - techniques: spectroscopic
Planets and satellites: individual: Jupiter
description Hydrocarbon species, and in particular CH4, play a key role in the stratosphere-thermosphere boundary of Jupiter, which occurs around the μ-bar pressure level. Previous analyses of solar occultation, He and Ly-α airglow, and ISO/SWS measurements of the radiance around 3.3 μm have inferred significantly different methane concentrations. Here we aim to accurately model the CH4 radiance at 3.3 μm measured by ISO/SWS by using a comprehensive non-local thermodynamic equilibrium model and the most recent collisional rates measured in the laboratory for CH4 to shed new light onto the methane concentration in the upper atmosphere of Jupiter. These emission bands have been shown to present a peak contribution precisely at the μ-bar level, hence directly probing the region of interest. We find that a high CH4 concentration is necessary to explain the data, in contrast with the most recent analyses, and that the observations favour the lower limit of the latest laboratory measurements of the CH4 collisional relaxation rates. Our results provide precise constraints on the composition and dynamics of the lower atmosphere of Jupiter. © ESO 2022.
publishDate 2022
dc.date.none.fl_str_mv 2022
2022
2022
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/285726
url http://hdl.handle.net/10261/285726
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MICINN//SEV-2017-0709
info:eu-repo/grantAgreement/EC/H2020/694513
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-110689RB-I00
http://dx.doi.org/10.1051/0004-6361/202141933
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
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