Photochemistry of Saturn's Atmosphere
Identifieur interne : 001F59 ( Istex/Corpus ); précédent : 001F58; suivant : 001F60Photochemistry of Saturn's Atmosphere
Auteurs : Julianne I. Moses ; Bruno Bézard ; Emmanuel Lellouch ; G. Randall Gladstone ; Helmut Feuchtgruber ; Mark AllenSource :
- Icarus [ 0019-1035 ] ; 2000.
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Abstract
To investigate the details of hydrocarbon photochemistry on Saturn, we have developed a one-dimensional diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation. The model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn's eddy diffusion coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn's upper atmosphere. From the ISO observations, we determine that the column densities of CH3, CH3C2H, and C4H2 above 10 mbar are 4+2−1.5×1013 cm−2, (1.1±0.3)×1015 cm−2, and (1.2±0.3)×1014 cm−2, respectively. The observed ISO emission features also indicate C2H2 mixing ratios of 1.2+0.9−0.6×10−6 at 0.3 mbar and (2.7±0.8)×10−7 at 1.4 mbar, and a C2H6 mixing ratio of (9±2.5)×10−6 at 0.5 mbar. Upper limits are provided for C2H4, CH2CCH2, C3H8, and C6H2. The sensitivity of the model results to variations in the eddy diffusion coefficient profile, the solar flux, the CH4 photolysis branching ratios, the atomic hydrogen influx, and key reaction rates are discussed in detail. We find that C4H2 and CH3C2H are particularly good tracers of important chemical processes and physical conditions in Saturn's upper atmosphere, and C2H6 is a good tracer of the eddy diffusion coefficient in Saturn's lower stratosphere. The eddy diffusion coefficient must be smaller than ∼3×104 cm2 s−1 at pressures greater than 1 mbar in order to reproduce the C2H6 abundance inferred from ISO observations. The eddy diffusion coefficients in the upper stratosphere could be constrained by observations of CH3 radicals if the low-temperature chemistry of CH3 were better understood. We also discuss the implications of our modeling for aerosol formation in Saturn's lower stratosphere—diacetylene, butane, and water condense between ∼1 and 300 mbar in our model and will dominate stratospheric haze formation at nonauroral latitudes. Our photochemical models will be useful for planning observational sequences and for analyzing data from the upcoming Cassini mission.
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DOI: 10.1006/icar.1999.6270
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Moses</name><affiliation><mods:affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas, 77058-1113, f1 moses@lpi3.jsc.nasa.govf1</mods:affiliation></affiliation></author><author><name sortKey="Bezard, Bruno" sort="Bezard, Bruno" uniqKey="Bezard B" first="Bruno" last="Bézard">Bruno Bézard</name><affiliation><mods:affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</mods:affiliation></affiliation></author><author><name sortKey="Lellouch, Emmanuel" sort="Lellouch, Emmanuel" uniqKey="Lellouch E" first="Emmanuel" last="Lellouch">Emmanuel Lellouch</name><affiliation><mods:affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</mods:affiliation></affiliation></author><author><name sortKey="Gladstone, G Randall" sort="Gladstone, G Randall" uniqKey="Gladstone G" first="G. Randall" last="Gladstone">G. Randall Gladstone</name><affiliation><mods:affiliation>Space Sciences Department, Southwest Research Institute, San Antonio, Texas, 78228-0510</mods:affiliation></affiliation></author><author><name sortKey="Feuchtgruber, Helmut" sort="Feuchtgruber, Helmut" uniqKey="Feuchtgruber H" first="Helmut" last="Feuchtgruber">Helmut Feuchtgruber</name><affiliation><mods:affiliation>Max-Planck Institut für Extraterrestrische Physik, Garching, 85740, Germany</mods:affiliation></affiliation></author><author><name sortKey="Allen, Mark" sort="Allen, Mark" uniqKey="Allen M" first="Mark" last="Allen">Mark Allen</name><affiliation><mods:affiliation>Earth and Space Science Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California, 91109</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:79FC56D1DA0A9235A3D8895F07188E2A3528818B</idno><date when="2000" year="2000">2000</date><idno type="doi">10.1006/icar.1999.6270</idno><idno type="url">https://api.istex.fr/document/79FC56D1DA0A9235A3D8895F07188E2A3528818B/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001F59</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001F59</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main" xml:lang="en">Photochemistry of Saturn's Atmosphere</title><author><name sortKey="Moses, Julianne I" sort="Moses, Julianne I" uniqKey="Moses J" first="Julianne I." last="Moses">Julianne I. Moses</name><affiliation><mods:affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas, 77058-1113, f1 moses@lpi3.jsc.nasa.govf1</mods:affiliation></affiliation></author><author><name sortKey="Bezard, Bruno" sort="Bezard, Bruno" uniqKey="Bezard B" first="Bruno" last="Bézard">Bruno Bézard</name><affiliation><mods:affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</mods:affiliation></affiliation></author><author><name sortKey="Lellouch, Emmanuel" sort="Lellouch, Emmanuel" uniqKey="Lellouch E" first="Emmanuel" last="Lellouch">Emmanuel Lellouch</name><affiliation><mods:affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</mods:affiliation></affiliation></author><author><name sortKey="Gladstone, G Randall" sort="Gladstone, G Randall" uniqKey="Gladstone G" first="G. Randall" last="Gladstone">G. Randall Gladstone</name><affiliation><mods:affiliation>Space Sciences Department, Southwest Research Institute, San Antonio, Texas, 78228-0510</mods:affiliation></affiliation></author><author><name sortKey="Feuchtgruber, Helmut" sort="Feuchtgruber, Helmut" uniqKey="Feuchtgruber H" first="Helmut" last="Feuchtgruber">Helmut Feuchtgruber</name><affiliation><mods:affiliation>Max-Planck Institut für Extraterrestrische Physik, Garching, 85740, Germany</mods:affiliation></affiliation></author><author><name sortKey="Allen, Mark" sort="Allen, Mark" uniqKey="Allen M" first="Mark" last="Allen">Mark Allen</name><affiliation><mods:affiliation>Earth and Space Science Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California, 91109</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Icarus</title><title level="j" type="abbrev">YICAR</title><idno type="ISSN">0019-1035</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="2000">2000</date><biblScope unit="volume">143</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="244">244</biblScope><biblScope unit="page" to="298">298</biblScope></imprint><idno type="ISSN">0019-1035</idno></series><idno type="istex">79FC56D1DA0A9235A3D8895F07188E2A3528818B</idno><idno type="DOI">10.1006/icar.1999.6270</idno><idno type="PII">S0019-1035(99)96270-X</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0019-1035</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Saturn</term><term>atmosphere</term><term>atmospheres</term><term>composition</term><term>infrared observations</term><term>organic chemistry</term><term>photochemistry</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">To investigate the details of hydrocarbon photochemistry on Saturn, we have developed a one-dimensional diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation. The model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn's eddy diffusion coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn's upper atmosphere. From the ISO observations, we determine that the column densities of CH3, CH3C2H, and C4H2 above 10 mbar are 4+2−1.5×1013 cm−2, (1.1±0.3)×1015 cm−2, and (1.2±0.3)×1014 cm−2, respectively. The observed ISO emission features also indicate C2H2 mixing ratios of 1.2+0.9−0.6×10−6 at 0.3 mbar and (2.7±0.8)×10−7 at 1.4 mbar, and a C2H6 mixing ratio of (9±2.5)×10−6 at 0.5 mbar. Upper limits are provided for C2H4, CH2CCH2, C3H8, and C6H2. The sensitivity of the model results to variations in the eddy diffusion coefficient profile, the solar flux, the CH4 photolysis branching ratios, the atomic hydrogen influx, and key reaction rates are discussed in detail. We find that C4H2 and CH3C2H are particularly good tracers of important chemical processes and physical conditions in Saturn's upper atmosphere, and C2H6 is a good tracer of the eddy diffusion coefficient in Saturn's lower stratosphere. The eddy diffusion coefficient must be smaller than ∼3×104 cm2 s−1 at pressures greater than 1 mbar in order to reproduce the C2H6 abundance inferred from ISO observations. The eddy diffusion coefficients in the upper stratosphere could be constrained by observations of CH3 radicals if the low-temperature chemistry of CH3 were better understood. We also discuss the implications of our modeling for aerosol formation in Saturn's lower stratosphere—diacetylene, butane, and water condense between ∼1 and 300 mbar in our model and will dominate stratospheric haze formation at nonauroral latitudes. Our photochemical models will be useful for planning observational sequences and for analyzing data from the upcoming Cassini mission.</div></front></TEI><istex><corpusName>elsevier</corpusName><author><json:item><name>Julianne I. Moses</name><affiliations><json:string>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas, 77058-1113, f1 moses@lpi3.jsc.nasa.govf1</json:string></affiliations></json:item><json:item><name>Bruno Bézard</name><affiliations><json:string>DESPA, Observatoire de Paris, Meudon, 92195, France</json:string></affiliations></json:item><json:item><name>Emmanuel Lellouch</name><affiliations><json:string>DESPA, Observatoire de Paris, Meudon, 92195, France</json:string></affiliations></json:item><json:item><name>G.Randall Gladstone</name><affiliations><json:string>Space Sciences Department, Southwest Research Institute, San Antonio, Texas, 78228-0510</json:string></affiliations></json:item><json:item><name>Helmut Feuchtgruber</name><affiliations><json:string>Max-Planck Institut für Extraterrestrische Physik, Garching, 85740, Germany</json:string></affiliations></json:item><json:item><name>Mark Allen</name><affiliations><json:string>Earth and Space Science Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California, 91109</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>Saturn</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>atmosphere</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>photochemistry</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>atmospheres</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>composition</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>organic chemistry</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>infrared observations</value></json:item></subject><language><json:string>eng</json:string></language><originalGenre><json:string>Full-length article</json:string></originalGenre><abstract>To investigate the details of hydrocarbon photochemistry on Saturn, we have developed a one-dimensional diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation. The model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn's eddy diffusion coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn's upper atmosphere. From the ISO observations, we determine that the column densities of CH3, CH3C2H, and C4H2 above 10 mbar are 4+2−1.5×1013 cm−2, (1.1±0.3)×1015 cm−2, and (1.2±0.3)×1014 cm−2, respectively. The observed ISO emission features also indicate C2H2 mixing ratios of 1.2+0.9−0.6×10−6 at 0.3 mbar and (2.7±0.8)×10−7 at 1.4 mbar, and a C2H6 mixing ratio of (9±2.5)×10−6 at 0.5 mbar. Upper limits are provided for C2H4, CH2CCH2, C3H8, and C6H2. The sensitivity of the model results to variations in the eddy diffusion coefficient profile, the solar flux, the CH4 photolysis branching ratios, the atomic hydrogen influx, and key reaction rates are discussed in detail. We find that C4H2 and CH3C2H are particularly good tracers of important chemical processes and physical conditions in Saturn's upper atmosphere, and C2H6 is a good tracer of the eddy diffusion coefficient in Saturn's lower stratosphere. The eddy diffusion coefficient must be smaller than ∼3×104 cm2 s−1 at pressures greater than 1 mbar in order to reproduce the C2H6 abundance inferred from ISO observations. The eddy diffusion coefficients in the upper stratosphere could be constrained by observations of CH3 radicals if the low-temperature chemistry of CH3 were better understood. We also discuss the implications of our modeling for aerosol formation in Saturn's lower stratosphere—diacetylene, butane, and water condense between ∼1 and 300 mbar in our model and will dominate stratospheric haze formation at nonauroral latitudes. Our photochemical models will be useful for planning observational sequences and for analyzing data from the upcoming Cassini mission.</abstract><qualityIndicators><score>8</score><pdfVersion>1.2</pdfVersion><pdfPageSize>543 x 758 pts</pdfPageSize><refBibsNative>true</refBibsNative><keywordCount>7</keywordCount><abstractCharCount>2215</abstractCharCount><pdfWordCount>35412</pdfWordCount><pdfCharCount>183913</pdfCharCount><pdfPageCount>55</pdfPageCount><abstractWordCount>322</abstractWordCount></qualityIndicators><title>Photochemistry of Saturn's Atmosphere</title><pii><json:string>S0019-1035(99)96270-X</json:string></pii><refBibs><json:item><author><json:item><name>U. Alkemade</name></json:item><json:item><name>K.H. Homann</name></json:item></author><host><volume>161</volume><pages><last>34</last><first>19</first></pages><author></author><title>Z. Phys. Chem. 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Hydrocarbon Chemistry and Comparisons with ISO Observations</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>ELSEVIER</publisher><availability><p>©2000 Academic Press</p></availability><date>2000</date></publicationStmt><notesStmt><note type="content">Section title: Regular Article</note></notesStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">Photochemistry of Saturn's Atmosphere</title><title level="a" type="sub" xml:lang="en">I. Hydrocarbon Chemistry and Comparisons with ISO Observations</title><author xml:id="author-1"><persName><forename type="first">Julianne I.</forename><surname>Moses</surname></persName><affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas, 77058-1113, f1 moses@lpi3.jsc.nasa.govf1</affiliation></author><author xml:id="author-2"><persName><forename type="first">Bruno</forename><surname>Bézard</surname></persName><affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</affiliation></author><author xml:id="author-3"><persName><forename type="first">Emmanuel</forename><surname>Lellouch</surname></persName><affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</affiliation></author><author xml:id="author-4"><persName><forename type="first">G.Randall</forename><surname>Gladstone</surname></persName><affiliation>Space Sciences Department, Southwest Research Institute, San Antonio, Texas, 78228-0510</affiliation></author><author xml:id="author-5"><persName><forename type="first">Helmut</forename><surname>Feuchtgruber</surname></persName><affiliation>Max-Planck Institut für Extraterrestrische Physik, Garching, 85740, Germany</affiliation></author><author xml:id="author-6"><persName><forename type="first">Mark</forename><surname>Allen</surname></persName><affiliation>Earth and Space Science Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California, 91109</affiliation></author></analytic><monogr><title level="j">Icarus</title><title level="j" type="abbrev">YICAR</title><idno type="pISSN">0019-1035</idno><idno type="PII">S0019-1035(00)X0021-8</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="2000"></date><biblScope unit="volume">143</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="244">244</biblScope><biblScope unit="page" to="298">298</biblScope></imprint></monogr><idno type="istex">79FC56D1DA0A9235A3D8895F07188E2A3528818B</idno><idno type="DOI">10.1006/icar.1999.6270</idno><idno type="PII">S0019-1035(99)96270-X</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2000</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>To investigate the details of hydrocarbon photochemistry on Saturn, we have developed a one-dimensional diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation. The model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn's eddy diffusion coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn's upper atmosphere. From the ISO observations, we determine that the column densities of CH3, CH3C2H, and C4H2 above 10 mbar are 4+2−1.5×1013 cm−2, (1.1±0.3)×1015 cm−2, and (1.2±0.3)×1014 cm−2, respectively. The observed ISO emission features also indicate C2H2 mixing ratios of 1.2+0.9−0.6×10−6 at 0.3 mbar and (2.7±0.8)×10−7 at 1.4 mbar, and a C2H6 mixing ratio of (9±2.5)×10−6 at 0.5 mbar. Upper limits are provided for C2H4, CH2CCH2, C3H8, and C6H2. The sensitivity of the model results to variations in the eddy diffusion coefficient profile, the solar flux, the CH4 photolysis branching ratios, the atomic hydrogen influx, and key reaction rates are discussed in detail. We find that C4H2 and CH3C2H are particularly good tracers of important chemical processes and physical conditions in Saturn's upper atmosphere, and C2H6 is a good tracer of the eddy diffusion coefficient in Saturn's lower stratosphere. The eddy diffusion coefficient must be smaller than ∼3×104 cm2 s−1 at pressures greater than 1 mbar in order to reproduce the C2H6 abundance inferred from ISO observations. The eddy diffusion coefficients in the upper stratosphere could be constrained by observations of CH3 radicals if the low-temperature chemistry of CH3 were better understood. We also discuss the implications of our modeling for aerosol formation in Saturn's lower stratosphere—diacetylene, butane, and water condense between ∼1 and 300 mbar in our model and will dominate stratospheric haze formation at nonauroral latitudes. Our photochemical models will be useful for planning observational sequences and for analyzing data from the upcoming Cassini mission.</p></abstract><textClass xml:lang="en"><keywords scheme="keyword"><list><head>Abbreviations</head><item><term>Saturn</term></item></list></keywords></textClass><textClass xml:lang="en"><keywords scheme="keyword"><list><head>Abbreviations</head><item><term>atmosphere</term></item></list></keywords></textClass><textClass xml:lang="en"><keywords scheme="keyword"><list><head>Abbreviations</head><item><term>photochemistry</term></item></list></keywords></textClass><textClass xml:lang="en"><keywords scheme="keyword"><list><head>Abbreviations</head><item><term>atmospheres</term></item></list></keywords></textClass><textClass xml:lang="en"><keywords scheme="keyword"><list><head>Abbreviations</head><item><term>composition</term></item></list></keywords></textClass><textClass xml:lang="en"><keywords scheme="keyword"><list><head>Abbreviations</head><item><term>organic chemistry</term></item></list></keywords></textClass><textClass xml:lang="en"><keywords scheme="keyword"><list><head>Abbreviations</head><item><term>infrared observations</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="1999-08-18">Modified</change><change when="2000">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/79FC56D1DA0A9235A3D8895F07188E2A3528818B/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Elsevier, elements deleted: tail"><istex:xmlDeclaration>version="1.0" encoding="utf-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//ES//DTD journal article DTD version 4.5.2//EN//XML" URI="art452.dtd" name="istex:docType"></istex:docType><istex:document><converted-article version="4.5.2" docsubtype="fla" xml:lang="en"><item-info><jid>YICAR</jid><aid>96270</aid><ce:pii>S0019-1035(99)96270-X</ce:pii><ce:doi>10.1006/icar.1999.6270</ce:doi><ce:copyright type="full-transfer" year="2000">Academic Press</ce:copyright></item-info><head><ce:dochead><ce:textfn>Regular Article</ce:textfn></ce:dochead><ce:title>Photochemistry of Saturn's Atmosphere</ce:title><ce:subtitle>I. Hydrocarbon Chemistry and Comparisons with ISO Observations</ce:subtitle><ce:author-group><ce:author><ce:given-name>Julianne I.</ce:given-name><ce:surname>Moses</ce:surname><ce:cross-ref refid="A0"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Bruno</ce:given-name><ce:surname>Bézard</ce:surname><ce:cross-ref refid="A1"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Emmanuel</ce:given-name><ce:surname>Lellouch</ce:surname><ce:cross-ref refid="A1"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>G.Randall</ce:given-name><ce:surname>Gladstone</ce:surname><ce:cross-ref refid="A2"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Helmut</ce:given-name><ce:surname>Feuchtgruber</ce:surname><ce:cross-ref refid="A3"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Mark</ce:given-name><ce:surname>Allen</ce:surname><ce:cross-ref refid="A4"><ce:sup>e</ce:sup></ce:cross-ref><ce:cross-ref refid="A5"><ce:sup>f</ce:sup></ce:cross-ref></ce:author><ce:affiliation id="A0"><ce:label>a</ce:label><ce:textfn>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas, 77058-1113, <ce:footnote id="F1"><ce:label>f1</ce:label><ce:note-para>moses@lpi3.jsc.nasa.gov</ce:note-para></ce:footnote><ce:cross-ref refid="F1"><ce:sup>f1</ce:sup></ce:cross-ref></ce:textfn></ce:affiliation><ce:affiliation id="A1"><ce:label>b</ce:label><ce:textfn>DESPA, Observatoire de Paris, Meudon, 92195, France</ce:textfn></ce:affiliation><ce:affiliation id="A2"><ce:label>c</ce:label><ce:textfn>Space Sciences Department, Southwest Research Institute, San Antonio, Texas, 78228-0510</ce:textfn></ce:affiliation><ce:affiliation id="A3"><ce:label>d</ce:label><ce:textfn>Max-Planck Institut für Extraterrestrische Physik, Garching, 85740, Germany</ce:textfn></ce:affiliation><ce:affiliation id="A4"><ce:label>e</ce:label><ce:textfn>Earth and Space Science Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California, 91109</ce:textfn></ce:affiliation><ce:affiliation id="A5"><ce:label>f</ce:label><ce:textfn>Division for Geological and Planetary Sciences, Caltech 170-25, Pasadena, California, 91125</ce:textfn></ce:affiliation></ce:author-group><ce:date-received day="18" month="2" year="1999"></ce:date-received><ce:date-revised day="18" month="8" year="1999"></ce:date-revised><ce:abstract><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>To investigate the details of hydrocarbon photochemistry on Saturn, we have developed a one-dimensional diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation. The model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn's eddy diffusion coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn's upper atmosphere. From the ISO observations, we determine that the column densities of CH<ce:inf>3</ce:inf>, CH<ce:inf>3</ce:inf>C<ce:inf>2</ce:inf>H, and C<ce:inf>4</ce:inf>H<ce:inf>2</ce:inf> above 10 mbar are 4<ce:sup>+2</ce:sup><ce:inf>−1.5</ce:inf>×10<ce:sup>13</ce:sup> cm<ce:sup>−2</ce:sup>, (1.1±0.3)×10<ce:sup>15</ce:sup> cm<ce:sup>−2</ce:sup>, and (1.2±0.3)×10<ce:sup>14</ce:sup> cm<ce:sup>−2</ce:sup>, respectively. The observed ISO emission features also indicate C<ce:inf>2</ce:inf>H<ce:inf>2</ce:inf> mixing ratios of 1.2<ce:sup>+0.9</ce:sup><ce:inf>−0.6</ce:inf>×10<ce:sup>−6</ce:sup> at 0.3 mbar and (2.7±0.8)×10<ce:sup>−7</ce:sup> at 1.4 mbar, and a C<ce:inf>2</ce:inf>H<ce:inf>6</ce:inf> mixing ratio of (9±2.5)×10<ce:sup>−6</ce:sup> at 0.5 mbar. Upper limits are provided for C<ce:inf>2</ce:inf>H<ce:inf>4</ce:inf>, CH<ce:inf>2</ce:inf>CCH<ce:inf>2</ce:inf>, C<ce:inf>3</ce:inf>H<ce:inf>8</ce:inf>, and C<ce:inf>6</ce:inf>H<ce:inf>2</ce:inf>. The sensitivity of the model results to variations in the eddy diffusion coefficient profile, the solar flux, the CH<ce:inf>4</ce:inf> photolysis branching ratios, the atomic hydrogen influx, and key reaction rates are discussed in detail. We find that C<ce:inf>4</ce:inf>H<ce:inf>2</ce:inf> and CH<ce:inf>3</ce:inf>C<ce:inf>2</ce:inf>H are particularly good tracers of important chemical processes and physical conditions in Saturn's upper atmosphere, and C<ce:inf>2</ce:inf>H<ce:inf>6</ce:inf> is a good tracer of the eddy diffusion coefficient in Saturn's lower stratosphere. The eddy diffusion coefficient must be smaller than ∼3×10<ce:sup>4</ce:sup> cm<ce:sup>2</ce:sup> s<ce:sup>−1</ce:sup> at pressures greater than 1 mbar in order to reproduce the C<ce:inf>2</ce:inf>H<ce:inf>6</ce:inf> abundance inferred from ISO observations. The eddy diffusion coefficients in the upper stratosphere could be constrained by observations of CH<ce:inf>3</ce:inf> radicals if the low-temperature chemistry of CH<ce:inf>3</ce:inf> were better understood. We also discuss the implications of our modeling for aerosol formation in Saturn's lower stratosphere—diacetylene, butane, and water condense between ∼1 and 300 mbar in our model and will dominate stratospheric haze formation at nonauroral latitudes. Our photochemical models will be useful for planning observational sequences and for analyzing data from the upcoming <ce:italic>Cassini</ce:italic> mission.</ce:simple-para></ce:abstract-sec></ce:abstract><ce:keywords class="abr"><ce:section-title>Abbreviations</ce:section-title><ce:keyword><ce:text>Saturn</ce:text></ce:keyword></ce:keywords><ce:keywords class="abr"><ce:section-title>Abbreviations</ce:section-title><ce:keyword><ce:text>atmosphere</ce:text></ce:keyword></ce:keywords><ce:keywords class="abr"><ce:section-title>Abbreviations</ce:section-title><ce:keyword><ce:text>photochemistry</ce:text></ce:keyword></ce:keywords><ce:keywords class="abr"><ce:section-title>Abbreviations</ce:section-title><ce:keyword><ce:text>atmospheres</ce:text></ce:keyword></ce:keywords><ce:keywords class="abr"><ce:section-title>Abbreviations</ce:section-title><ce:keyword><ce:text>composition</ce:text></ce:keyword></ce:keywords><ce:keywords class="abr"><ce:section-title>Abbreviations</ce:section-title><ce:keyword><ce:text>organic chemistry</ce:text></ce:keyword></ce:keywords><ce:keywords class="abr"><ce:section-title>Abbreviations</ce:section-title><ce:keyword><ce:text>infrared observations</ce:text></ce:keyword></ce:keywords></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Photochemistry of Saturn's Atmosphere</title><subTitle>I. Hydrocarbon Chemistry and Comparisons with ISO Observations</subTitle></titleInfo><titleInfo type="alternative" lang="en" contentType="CDATA"><title>Photochemistry of Saturn's Atmosphere</title><subTitle>I. Hydrocarbon Chemistry and Comparisons with ISO Observations</subTitle></titleInfo><name type="personal"><namePart type="given">Julianne I.</namePart><namePart type="family">Moses</namePart><affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas, 77058-1113, f1 moses@lpi3.jsc.nasa.govf1</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Bruno</namePart><namePart type="family">Bézard</namePart><affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Emmanuel</namePart><namePart type="family">Lellouch</namePart><affiliation>DESPA, Observatoire de Paris, Meudon, 92195, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.Randall</namePart><namePart type="family">Gladstone</namePart><affiliation>Space Sciences Department, Southwest Research Institute, San Antonio, Texas, 78228-0510</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Helmut</namePart><namePart type="family">Feuchtgruber</namePart><affiliation>Max-Planck Institut für Extraterrestrische Physik, Garching, 85740, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Mark</namePart><namePart type="family">Allen</namePart><affiliation>Earth and Space Science Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California, 91109</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="research-article" displayLabel="Full-length article"></genre><originInfo><publisher>ELSEVIER</publisher><dateIssued encoding="w3cdtf">2000</dateIssued><dateModified encoding="w3cdtf">1999-08-18</dateModified><copyrightDate encoding="w3cdtf">2000</copyrightDate></originInfo><language><languageTerm type="code" authority="iso639-2b">eng</languageTerm><languageTerm type="code" authority="rfc3066">en</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType></physicalDescription><abstract lang="en">To investigate the details of hydrocarbon photochemistry on Saturn, we have developed a one-dimensional diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation. The model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn's eddy diffusion coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn's upper atmosphere. From the ISO observations, we determine that the column densities of CH3, CH3C2H, and C4H2 above 10 mbar are 4+2−1.5×1013 cm−2, (1.1±0.3)×1015 cm−2, and (1.2±0.3)×1014 cm−2, respectively. The observed ISO emission features also indicate C2H2 mixing ratios of 1.2+0.9−0.6×10−6 at 0.3 mbar and (2.7±0.8)×10−7 at 1.4 mbar, and a C2H6 mixing ratio of (9±2.5)×10−6 at 0.5 mbar. Upper limits are provided for C2H4, CH2CCH2, C3H8, and C6H2. The sensitivity of the model results to variations in the eddy diffusion coefficient profile, the solar flux, the CH4 photolysis branching ratios, the atomic hydrogen influx, and key reaction rates are discussed in detail. We find that C4H2 and CH3C2H are particularly good tracers of important chemical processes and physical conditions in Saturn's upper atmosphere, and C2H6 is a good tracer of the eddy diffusion coefficient in Saturn's lower stratosphere. The eddy diffusion coefficient must be smaller than ∼3×104 cm2 s−1 at pressures greater than 1 mbar in order to reproduce the C2H6 abundance inferred from ISO observations. The eddy diffusion coefficients in the upper stratosphere could be constrained by observations of CH3 radicals if the low-temperature chemistry of CH3 were better understood. We also discuss the implications of our modeling for aerosol formation in Saturn's lower stratosphere—diacetylene, butane, and water condense between ∼1 and 300 mbar in our model and will dominate stratospheric haze formation at nonauroral latitudes. Our photochemical models will be useful for planning observational sequences and for analyzing data from the upcoming Cassini mission.</abstract><note type="content">Section title: Regular Article</note><subject lang="en"><genre>Abbreviations</genre><topic>Saturn</topic></subject><subject lang="en"><genre>Abbreviations</genre><topic>atmosphere</topic></subject><subject lang="en"><genre>Abbreviations</genre><topic>photochemistry</topic></subject><subject lang="en"><genre>Abbreviations</genre><topic>atmospheres</topic></subject><subject lang="en"><genre>Abbreviations</genre><topic>composition</topic></subject><subject lang="en"><genre>Abbreviations</genre><topic>organic chemistry</topic></subject><subject lang="en"><genre>Abbreviations</genre><topic>infrared observations</topic></subject><relatedItem type="host"><titleInfo><title>Icarus</title></titleInfo><titleInfo type="abbreviated"><title>YICAR</title></titleInfo><genre type="journal">journal</genre><originInfo><dateIssued encoding="w3cdtf">200002</dateIssued></originInfo><identifier type="ISSN">0019-1035</identifier><identifier type="PII">S0019-1035(00)X0021-8</identifier><part><date>200002</date><detail type="volume"><number>143</number><caption>vol.</caption></detail><detail type="issue"><number>2</number><caption>no.</caption></detail><extent unit="issue pages"><start>189</start><end>435</end></extent><extent unit="pages"><start>244</start><end>298</end></extent></part></relatedItem><identifier type="istex">79FC56D1DA0A9235A3D8895F07188E2A3528818B</identifier><identifier type="DOI">10.1006/icar.1999.6270</identifier><identifier type="PII">S0019-1035(99)96270-X</identifier><accessCondition type="use and reproduction" contentType="copyright">©2000 Academic Press</accessCondition><recordInfo><recordContentSource>ELSEVIER</recordContentSource><recordOrigin>Academic Press, ©2000</recordOrigin></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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