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dc.contributor.authorSchneider, Nicholases_ES
dc.contributor.authorMilby, Z.es_ES
dc.contributor.authorJain, S. K.es_ES
dc.contributor.authorGonzález-Galindo, F.es_ES
dc.contributor.authorRoyer, E.es_ES
dc.contributor.authorGérard, Jean-Claudees_ES
dc.contributor.authorStiepen, A.es_ES
dc.contributor.authorDeighan, J.es_ES
dc.contributor.authorStewart, A. I. F.es_ES
dc.contributor.authorForget, F.es_ES
dc.contributor.authorLefèvre, F.es_ES
dc.contributor.authorBougher, S.W.es_ES
dc.date.accessioned2020-09-04T11:58:41Z-
dc.date.available2020-09-04T11:58:41Z-
dc.date.issued2020-08-05-
dc.identifier.citationJournal of Geophysical Research - Part A - Space Physics 125(8): e2019JA027318 (2020)es_ES
dc.identifier.issn2169-9380-
dc.identifier.urihttp://hdl.handle.net/10261/219162-
dc.description.abstractWe report results from a study of two consecutive Martian years of imaging observations of nitric oxide ultraviolet nightglow by the Imaging Ultraviolet Spectrograph (IUVS) on the Mars Atmosphere and Volatile Evolution (MAVEN) mission spacecraft. The emission arises from recombination of N and O atoms in Mars' nightside mesosphere. The brightness traces the reaction rate as opposed to the abundance of constituents, revealing where circulation patterns concentrate N and O and enhance recombination. Emissions are brightest around the winter poles, with equatorial regions brightening around the equinoxes. These changes offer clear evidence of circulation patterns transitioning from a single cross-equatorial cell operating during solstice periods to more symmetric equator-to-poles circulation around the equinoxes. Prominent atmospheric tides intensify the emissions at different longitudes, latitude ranges, and seasons. We find a strong eastward-propagating diurnal tide (DE2) near the equator during the equinoxes, with a remarkably bright spot narrowly confined near (0°, 0°). Wave features at the opposite winter poles are dissimilar, reflecting different circulation patterns at perihelion versus aphelion. LMD-MGCM simulations agree with the patterns of most observed phenomena, confirming that the model captures the dominant physical processes. At the south winter pole, however, the model fails to match a strong wave-1 spiral feature. Observed brightnesses exceed model predictions by a factor of 1.9 globally, probably due to an underestimation of the dayside production of N and O atoms. Further study of discrepancies between the model and observations offers opportunities to improve our understanding of chemical and transport processes controlling the emission. ©2020. American Geophysical Union. All Rights Reserved.es_ES
dc.description.sponsorshipThe MAVEN mission is supported by NASA through the Mars Exploration Program in association with the University of Colorado and NASA's Goddard Space Flight Center. A. Stiepen was supported by the Fund for Scientific Research (F.R.S.‐FNRS). J.‐C. Gérard acknowledges support from the PRODEX program of the Belgian Federal Science Policy Office, managed by ESA. F. González‐Galindo was funded by the Spanish Ministry of Science, Innovation, and Universities, the Spanish State Agency for Research, and by EC FEDER funds under Grants ESP2017‐87143‐R and RTI2018‐100920‐J‐I00 and through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV‐2017‐0709).es_ES
dc.language.isoenges_ES
dc.publisherAmerican Geophysical Uniones_ES
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/SEV-2017-0709es_ES
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/RTI2018-100920-J-I00es_ES
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020//ESP2017-87143-Res_ES
dc.relation.isversionofPublisher's versiones_ES
dc.rightsopenAccessen_EN
dc.subjectAtmospherees_ES
dc.subjectCirculationes_ES
dc.subjectMarses_ES
dc.subjectNightglowes_ES
dc.subjectTideses_ES
dc.subjectUltravioletes_ES
dc.titleImaging of Martian Circulation Patterns and Atmospheric Tides Through MAVEN/IUVS Nightglow Observationses_ES
dc.typeartículoes_ES
dc.identifier.doi10.1029/2019JA027318-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1029/2019JA027318es_ES
dc.embargo.terms2021-02-05es_ES
dc.contributor.funderNational Aeronautics and Space Administration (US)es_ES
dc.contributor.funderUniversity of Coloradoes_ES
dc.contributor.funderFonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles)es_ES
dc.contributor.funderBelgian Science Policy Officees_ES
dc.contributor.funderMinisterio de Ciencia, Innovación y Universidades (España)es_ES
dc.contributor.funderEuropean Commissiones_ES
dc.relation.csices_ES
oprm.item.hasRevisionno ko 0 false*
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100010174es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100002661es_ES
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
item.openairetypeartículo-
item.cerifentitytypePublications-
item.fulltextWith Fulltext-
item.languageiso639-1en-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.grantfulltextopen-
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