Modeled O2 nightglow distributions in the Venusian atmosphere
Identifieur interne : 001718 ( Istex/Corpus ); précédent : 001717; suivant : 001719Modeled O2 nightglow distributions in the Venusian atmosphere
Auteurs : Marie-Ève Gagné ; Stella M. L. Melo ; Amanda S. Brecht ; Stephen W. Bougher ; Kimberly StrongSource :
- Journal of Geophysical Research: Planets [ 0148-0227 ] ; 2012-12.
Abstract
In this paper, we study the global distribution of the O2Infrared Atmospheric (0‐0) emission at 1.27μm in the Venusian atmosphere with an airglow model in combination with atmospheric conditions provided by a three‐dimensional model, the Venus Thermospheric Global Circulation Model. We compare our model simulations with airglow observations of this emission from the Visible and InfraRed Thermal Imaging Spectrometer on board the Venus Express orbiter. Our model is successful in reproducing the latitudinal and temporal trends seen in the observations for latitudes between 0° and 30°, while poleward of 30°, the model results start to diverge away from the measurements. We attribute this discrepancy to the atomic oxygen distribution at these latitudes in our model that is inconsistent with the recent measurements. We also conducted a sensitivity study to explore the dependence of the vertical structure and the distribution of the airglow emission on the atmospheric conditions. The sensitivity study confirms that changes in the distribution of atomic oxygen significantly affect the characteristics of the airglow layer. Therefore, meaningful comparisons with observations require a three‐dimensional model, which accounts for dynamical variations in the background atmosphere. With this investigation, we highlight the impact of the atmospheric conditions on the airglow distribution, which is important for the understanding of how the phenomenon plays.
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DOI: 10.1029/2012JE004102
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Res.</title><idno type="ISSN">0148-0227</idno><idno type="eISSN">2156-2202</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><date type="published" when="2012-12">2012-12</date><biblScope unit="volume">117</biblScope><biblScope unit="issue">E12</biblScope><biblScope unit="page" from="/">n/a</biblScope><biblScope unit="page" to="/">n/a</biblScope></imprint><idno type="ISSN">0148-0227</idno></series><idno type="istex">48C19996D7A7139FA31A1CB92214C0863B8261DE</idno><idno type="DOI">10.1029/2012JE004102</idno><idno type="ArticleID">2012JE004102</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0148-0227</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract">In this paper, we study the global distribution of the O2Infrared Atmospheric (0‐0) emission at 1.27μm in the Venusian atmosphere with an airglow model in combination with atmospheric conditions provided by a three‐dimensional model, the Venus Thermospheric Global Circulation Model. We compare our model simulations with airglow observations of this emission from the Visible and InfraRed Thermal Imaging Spectrometer on board the Venus Express orbiter. Our model is successful in reproducing the latitudinal and temporal trends seen in the observations for latitudes between 0° and 30°, while poleward of 30°, the model results start to diverge away from the measurements. We attribute this discrepancy to the atomic oxygen distribution at these latitudes in our model that is inconsistent with the recent measurements. We also conducted a sensitivity study to explore the dependence of the vertical structure and the distribution of the airglow emission on the atmospheric conditions. The sensitivity study confirms that changes in the distribution of atomic oxygen significantly affect the characteristics of the airglow layer. Therefore, meaningful comparisons with observations require a three‐dimensional model, which accounts for dynamical variations in the background atmosphere. 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We compare our model simulations with airglow observations of this emission from the Visible and InfraRed Thermal Imaging Spectrometer on board the Venus Express orbiter. Our model is successful in reproducing the latitudinal and temporal trends seen in the observations for latitudes between 0° and 30°, while poleward of 30°, the model results start to diverge away from the measurements. We attribute this discrepancy to the atomic oxygen distribution at these latitudes in our model that is inconsistent with the recent measurements. We also conducted a sensitivity study to explore the dependence of the vertical structure and the distribution of the airglow emission on the atmospheric conditions. The sensitivity study confirms that changes in the distribution of atomic oxygen significantly affect the characteristics of the airglow layer. Therefore, meaningful comparisons with observations require a three‐dimensional model, which accounts for dynamical variations in the background atmosphere. With this investigation, we highlight the impact of the atmospheric conditions on the airglow distribution, which is important for the understanding of how the phenomenon plays.</p></abstract><abstract style="short"><p>First model simulations of O2 airglow on Venus using a 3D GCM The model results compare well with the VIRTIS measurements at low latitudes Impact of atmospheric conditions on airglow structure is considerable</p></abstract><textClass><keywords scheme="keyword"><list><head>keywords</head><item><term>Venus</term></item><item><term>airglow</term></item><item><term>atmosphere</term></item><item><term>modeling</term></item><item><term>oxygen</term></item><item><term>photochemistry</term></item></list></keywords></textClass><textClass><keywords scheme="Journal Subject"><list><head>index-terms</head><item><term>ATMOSPHERIC COMPOSITION AND STRUCTURE</term></item><item><term>Middle atmosphere: composition and chemistry</term></item><item><term>Middle atmosphere: constituent transport and chemistry</term></item><item><term>Planetary atmospheres</term></item><item><term>Planetary atmospheres</term></item><item><term>GEOCHEMISTRY</term></item><item><term>Planetary geochemistry</term></item><item><term>ATMOSPHERIC PROCESSES</term></item><item><term>Middle atmosphere dynamics</term></item><item><term>PLANETARY SCIENCES: ASTROBIOLOGY</term></item><item><term>Planetary atmospheres, clouds, and hazes</term></item><item><term>PLANETARY SCIENCES: SOLID SURFACE PLANETS</term></item><item><term>Atmospheres</term></item><item><term>Aurorae and airglow</term></item><item><term>Atmospheres</term></item><item><term>PLANETARY SCIENCES: FLUID PLANETS</term></item><item><term>Atmospheres</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2012-04-11">Received</change><change when="2012-10-14">Registration</change><change when="2012-12">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api-v5.istex.fr/document/48C19996D7A7139FA31A1CB92214C0863B8261DE/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component type="serialArticle" version="2.0" xml:lang="en" xml:id="jgre3128"><header><publicationMeta level="product"><doi>10.1002/(ISSN)2156-2202e</doi><issn type="print">0148-0227</issn><issn type="electronic">2156-2202</issn><idGroup><id type="product" value="JGRE"></id><id type="coden" value="JGREA2"></id></idGroup><titleGroup><title type="main" xml:lang="en" sort="JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS">Journal of Geophysical Research: Planets</title><title type="short">J. 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Gagné, Space Science and Technology, Canadian Space Agency, Saint‐Hubert, QC J3Y 8Y9, Canada. (<email>megagne@atmosp.physics.utoronto.ca</email>)</correspondenceTo><subjectInfo><subject href="http://psi.agu.org/taxonomy5/0300">ATMOSPHERIC COMPOSITION AND STRUCTURE</subject><subjectInfo><subject href="http://psi.agu.org/taxonomy5/0340">Middle atmosphere: composition and chemistry</subject><subject href="http://psi.agu.org/taxonomy5/0341">Middle atmosphere: constituent transport and chemistry</subject><subject href="http://psi.agu.org/taxonomy5/0343">Planetary atmospheres</subject><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/0343">Planetary atmospheres</subject></subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/1000">GEOCHEMISTRY</subject><subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/1060">Planetary geochemistry</subject></subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/3300">ATMOSPHERIC PROCESSES</subject><subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/3334">Middle atmosphere dynamics</subject></subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/5200">PLANETARY SCIENCES: ASTROBIOLOGY</subject><subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/5210">Planetary atmospheres, clouds, and hazes</subject></subjectInfo><subject href="http://psi.agu.org/taxonomy5/5400">PLANETARY SCIENCES: SOLID SURFACE PLANETS</subject><subjectInfo><subject href="http://psi.agu.org/taxonomy5/5405">Atmospheres</subject><subject href="http://psi.agu.org/taxonomy5/5408">Aurorae and airglow</subject><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/5405">Atmospheres</subject></subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/5700">PLANETARY SCIENCES: FLUID PLANETS</subject><subjectInfo><subject role="crossTerm" href="http://psi.agu.org/taxonomy5/5704">Atmospheres</subject></subjectInfo></subjectInfo><selfCitationGroup><citation xml:id="jgre3128-cit-0000" type="self"><author><familyName>Gagné</familyName>, <givenNames>M.‐È.</givenNames></author>, <author><givenNames>S. M. L.</givenNames> <familyName>Melo</familyName></author>, <author><givenNames>A. S.</givenNames> <familyName>Brecht</familyName></author>, <author><givenNames>S. W.</givenNames> <familyName>Bougher</familyName></author>, <author><givenNames>K.</givenNames> <familyName>Strong</familyName></author> (<pubYear year="2012">2012</pubYear>), <articleTitle>Modeled O<sub>2</sub> nightglow distributions in the Venusian atmosphere</articleTitle>, <journalTitle>J. Geophys. Res.</journalTitle>, <vol>117</vol>, E12002, doi:<accessionId ref="info:doi/10.1029/2012JE004102">10.1029/2012JE004102</accessionId>.</citation></selfCitationGroup><linkGroup><link type="toTypesetVersion" href="file:JGRE.JGRE3128.pdf"></link></linkGroup></publicationMeta><contentMeta><countGroup><count type="wordTotal" number="8500"></count><count type="figureTotal" number="5"></count><count type="tableTotal" number="1"></count></countGroup><titleGroup><title type="main">Modeled O<sub>2</sub> nightglow distributions in the Venusian atmosphere</title><title type="shortAuthors">GAGNÉ ET AL.</title><title type="short">O<sub>2</sub> NIGHTGLOW IN VENUS ATMOSPHERE</title></titleGroup><creators><creator xml:id="jgre3128-cr-0001" creatorRole="author" affiliationRef="#jgre3128-aff-0001 #jgre3128-aff-0002" corresponding="yes"><personName><givenNames>Marie‐Ève</givenNames><familyName>Gagné</familyName></personName><contactDetails><email>megagne@atmosp.physics.utoronto.ca</email></contactDetails></creator><creator xml:id="jgre3128-cr-0002" creatorRole="author" affiliationRef="#jgre3128-aff-0001"><personName><givenNames>Stella M. L.</givenNames><familyName>Melo</familyName></personName></creator><creator xml:id="jgre3128-cr-0003" creatorRole="author" affiliationRef="#jgre3128-aff-0003"><personName><givenNames>Amanda S.</givenNames><familyName>Brecht</familyName></personName></creator><creator xml:id="jgre3128-cr-0004" creatorRole="author" affiliationRef="#jgre3128-aff-0004"><personName><givenNames>Stephen W.</givenNames><familyName>Bougher</familyName></personName></creator><creator xml:id="jgre3128-cr-0005" creatorRole="author" affiliationRef="#jgre3128-aff-0002"><personName><givenNames>Kimberly</givenNames><familyName>Strong</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="jgre3128-aff-0001" countryCode="CA" type="organization"><unparsedAffiliation>Space Science and Technology, Canadian Space Agency, Saint-Hubert, Quebec, Canada</unparsedAffiliation></affiliation><affiliation xml:id="jgre3128-aff-0002" countryCode="CA" type="organization"><unparsedAffiliation>Department of Physics, University of Toronto, Toronto, Ontario, Canada</unparsedAffiliation></affiliation><affiliation xml:id="jgre3128-aff-0003" countryCode="US" type="organization"><unparsedAffiliation>Planetary System Branch, NASA Ames Research Center, Moffett Field, California, USA</unparsedAffiliation></affiliation><affiliation xml:id="jgre3128-aff-0004" countryCode="US" type="organization"><unparsedAffiliation>Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, Michigan, USA</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup type="author"><keyword xml:id="jgre3128-kwd-0001">Venus</keyword><keyword xml:id="jgre3128-kwd-0002">airglow</keyword><keyword xml:id="jgre3128-kwd-0003">atmosphere</keyword><keyword xml:id="jgre3128-kwd-0004">modeling</keyword><keyword xml:id="jgre3128-kwd-0005">oxygen</keyword><keyword xml:id="jgre3128-kwd-0006">photochemistry</keyword></keywordGroup><supportingInformation><supportingInfoItem><mediaResource alt="supplementary data" mimeType="text/plain" href="urn-x:wiley:01480227:media:jgre3128:jgre3128-sup-0001-t01"></mediaResource><caption>Tab‐delimited Table 1.</caption></supportingInfoItem></supportingInformation><abstractGroup><abstract type="main"><p xml:id="jgre3128-para-0001" label="1">In this paper, we study the global distribution of the O<sub>2</sub>Infrared Atmospheric (0‐0) emission at 1.27<i>μ</i>m in the Venusian atmosphere with an airglow model in combination with atmospheric conditions provided by a three‐dimensional model, the Venus Thermospheric Global Circulation Model. We compare our model simulations with airglow observations of this emission from the Visible and InfraRed Thermal Imaging Spectrometer on board the Venus Express orbiter. Our model is successful in reproducing the latitudinal and temporal trends seen in the observations for latitudes between 0° and 30°, while poleward of 30°, the model results start to diverge away from the measurements. We attribute this discrepancy to the atomic oxygen distribution at these latitudes in our model that is inconsistent with the recent measurements. We also conducted a sensitivity study to explore the dependence of the vertical structure and the distribution of the airglow emission on the atmospheric conditions. The sensitivity study confirms that changes in the distribution of atomic oxygen significantly affect the characteristics of the airglow layer. Therefore, meaningful comparisons with observations require a three‐dimensional model, which accounts for dynamical variations in the background atmosphere. With this investigation, we highlight the impact of the atmospheric conditions on the airglow distribution, which is important for the understanding of how the phenomenon plays.</p></abstract><abstract type="short"><title type="main">Key Points</title><p xml:id="jgre3128-para-0002"><list style="bulleted"><listItem>First model simulations of O2 airglow on Venus using a 3D GCM</listItem><listItem>The model results compare well with the VIRTIS measurements at low latitudes</listItem><listItem>Impact of atmospheric conditions on airglow structure is considerable</listItem></list></p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Modeled O2 nightglow distributions in the Venusian atmosphere</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>O2 NIGHTGLOW IN VENUS ATMOSPHERE</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Modeled O2 nightglow distributions in the Venusian atmosphere</title></titleInfo><name type="personal"><namePart type="given">Marie‐Ève</namePart><namePart type="family">Gagné</namePart><affiliation>Space Science and Technology, Canadian Space Agency, Saint-Hubert, Quebec, Canada</affiliation><affiliation>Department of Physics, University of Toronto, Toronto, Ontario, Canada</affiliation><affiliation>E-mail: megagne@atmosp.physics.utoronto.ca</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Stella M. L.</namePart><namePart type="family">Melo</namePart><affiliation>Space Science and Technology, Canadian Space Agency, Saint-Hubert, Quebec, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Amanda S.</namePart><namePart type="family">Brecht</namePart><affiliation>Planetary System Branch, NASA Ames Research Center, Moffett Field, California, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Stephen W.</namePart><namePart type="family">Bougher</namePart><affiliation>Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, Michigan, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Kimberly</namePart><namePart type="family">Strong</namePart><affiliation>Department of Physics, University of Toronto, Toronto, Ontario, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><dateIssued encoding="w3cdtf">2012-12</dateIssued><dateCaptured encoding="w3cdtf">2012-04-11</dateCaptured><dateValid encoding="w3cdtf">2012-10-14</dateValid><edition>Gagné, M.‐È., S. M. L. Melo, A. S. Brecht, S. W. Bougher, K. Strong (2012), Modeled O2 nightglow distributions in the Venusian atmosphere, J. Geophys. Res., 117, E12002, doi:10.1029/2012JE004102.</edition><copyrightDate encoding="w3cdtf">2012</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType><extent unit="figures">5</extent><extent unit="tables">1</extent><extent unit="words">8500</extent></physicalDescription><abstract>In this paper, we study the global distribution of the O2Infrared Atmospheric (0‐0) emission at 1.27μm in the Venusian atmosphere with an airglow model in combination with atmospheric conditions provided by a three‐dimensional model, the Venus Thermospheric Global Circulation Model. We compare our model simulations with airglow observations of this emission from the Visible and InfraRed Thermal Imaging Spectrometer on board the Venus Express orbiter. Our model is successful in reproducing the latitudinal and temporal trends seen in the observations for latitudes between 0° and 30°, while poleward of 30°, the model results start to diverge away from the measurements. We attribute this discrepancy to the atomic oxygen distribution at these latitudes in our model that is inconsistent with the recent measurements. We also conducted a sensitivity study to explore the dependence of the vertical structure and the distribution of the airglow emission on the atmospheric conditions. The sensitivity study confirms that changes in the distribution of atomic oxygen significantly affect the characteristics of the airglow layer. Therefore, meaningful comparisons with observations require a three‐dimensional model, which accounts for dynamical variations in the background atmosphere. With this investigation, we highlight the impact of the atmospheric conditions on the airglow distribution, which is important for the understanding of how the phenomenon plays.</abstract><abstract type="short">First model simulations of O2 airglow on Venus using a 3D GCM The model results compare well with the VIRTIS measurements at low latitudes Impact of atmospheric conditions on airglow structure is considerable</abstract><note type="additional physical form">Tab‐delimited Table 1.</note><subject><genre>keywords</genre><topic>Venus</topic><topic>airglow</topic><topic>atmosphere</topic><topic>modeling</topic><topic>oxygen</topic><topic>photochemistry</topic></subject><relatedItem type="host"><titleInfo><title>Journal of Geophysical Research: Planets</title></titleInfo><titleInfo type="abbreviated"><title>J. Geophys. Res.</title></titleInfo><genre type="journal">journal</genre><subject><genre>index-terms</genre><topic authorityURI="http://psi.agu.org/taxonomy5/0300">ATMOSPHERIC COMPOSITION AND STRUCTURE</topic><topic authorityURI="http://psi.agu.org/taxonomy5/0340">Middle atmosphere: composition and chemistry</topic><topic authorityURI="http://psi.agu.org/taxonomy5/0341">Middle atmosphere: constituent transport and chemistry</topic><topic authorityURI="http://psi.agu.org/taxonomy5/0343">Planetary atmospheres</topic><topic authorityURI="http://psi.agu.org/taxonomy5/0343">Planetary atmospheres</topic><topic authorityURI="http://psi.agu.org/taxonomy5/1000">GEOCHEMISTRY</topic><topic authorityURI="http://psi.agu.org/taxonomy5/1060">Planetary geochemistry</topic><topic authorityURI="http://psi.agu.org/taxonomy5/3300">ATMOSPHERIC PROCESSES</topic><topic authorityURI="http://psi.agu.org/taxonomy5/3334">Middle atmosphere dynamics</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5200">PLANETARY SCIENCES: ASTROBIOLOGY</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5210">Planetary atmospheres, clouds, and hazes</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5400">PLANETARY SCIENCES: SOLID SURFACE PLANETS</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5405">Atmospheres</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5408">Aurorae and airglow</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5405">Atmospheres</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5700">PLANETARY SCIENCES: FLUID PLANETS</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5704">Atmospheres</topic></subject><identifier type="ISSN">0148-0227</identifier><identifier type="eISSN">2156-2202</identifier><identifier type="DOI">10.1002/(ISSN)2156-2202e</identifier><identifier type="CODEN">JGREA2</identifier><identifier type="PublisherID">JGRE</identifier><part><date>2012</date><detail type="volume"><caption>vol.</caption><number>117</number></detail><detail type="issue"><caption>no.</caption><number>E12</number></detail><extent unit="pages"><start>n/a</start><end>n/a</end><total>10</total></extent></part></relatedItem><identifier type="istex">48C19996D7A7139FA31A1CB92214C0863B8261DE</identifier><identifier type="DOI">10.1029/2012JE004102</identifier><identifier type="ArticleID">2012JE004102</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2012 by the American Geophysical Union</accessCondition><recordInfo><recordContentSource>WILEY</recordContentSource></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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