On the Latitude Variation of Ammonia, Acetylene, and Phosphine Altitude Profiles on Jupiter from HST Faint Object Spectrograph Observations
Identifieur interne : 002626 ( Istex/Corpus ); précédent : 002625; suivant : 002627On the Latitude Variation of Ammonia, Acetylene, and Phosphine Altitude Profiles on Jupiter from HST Faint Object Spectrograph Observations
Auteurs : S. G. Edgington ; S. K. Atreya ; L. M. Trafton ; J. J. Caldwell ; R. F. Beebe ; A. A. Simon ; R. A. West ; C. BarnetSource :
- Icarus [ 0019-1035 ] ; 1998.
Abstract
Ultraviolet spectra in the spectral region from 160 to 230 nm were taken with the Hubble Space Telescope Faint Object Spectrograph in May 1992. We analyze these data to obtain the altitude distribution of ammonia and its variation with latitude from 6°N to 25°N. Ammonia condenses below the 150-mbar level, above which it departs from saturation due to photolysis. Using a photochemical model, we also derive the value of atmospheric eddy mixing coefficients at the observed latitudes. It is found that the eddy diffusion coefficient varies from 1.5 × 104cm2s−1at 450 mbar to 4.9 × 102cm2s−1at 120 mbar. The vertical distribution of ammonia and the eddy diffusion coefficient do not show a large variation with latitude. We also determine an acetylene mixing ratio of (10–30) × 10−9near 80 mbar and an upper limit of 1.5 × 10−7for the phosphine mixing ratio, if PH3is mixed uniformly below the 140 mbar level. The existence of particulate haze at low and high latitudes is also investigated.
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DOI: 10.1006/icar.1998.5925
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We analyze these data to obtain the altitude distribution of ammonia and its variation with latitude from 6°N to 25°N. Ammonia condenses below the 150-mbar level, above which it departs from saturation due to photolysis. Using a photochemical model, we also derive the value of atmospheric eddy mixing coefficients at the observed latitudes. It is found that the eddy diffusion coefficient varies from 1.5 × 104cm2s−1at 450 mbar to 4.9 × 102cm2s−1at 120 mbar. The vertical distribution of ammonia and the eddy diffusion coefficient do not show a large variation with latitude. We also determine an acetylene mixing ratio of (10–30) × 10−9near 80 mbar and an upper limit of 1.5 × 10−7for the phosphine mixing ratio, if PH3is mixed uniformly below the 140 mbar level. The existence of particulate haze at low and high latitudes is also investigated.</p></abstract></profileDesc><revisionDesc><change when="1998-02-05">Modified</change><change when="1998">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/5CF2D76DE67CFA0351443AF354FB9B2F0AC05D64/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>95925</aid><ce:pii>S0019-1035(98)95925-5</ce:pii><ce:doi>10.1006/icar.1998.5925</ce:doi><ce:copyright type="full-transfer" year="1998">Academic Press</ce:copyright></item-info><head><ce:article-footnote><ce:label>☆</ce:label><ce:note-para>G. E. Hunt</ce:note-para></ce:article-footnote><ce:dochead><ce:textfn>Regular Article</ce:textfn></ce:dochead><ce:title>On the Latitude Variation of Ammonia, Acetylene, and Phosphine Altitude Profiles on Jupiter from HST Faint Object Spectrograph Observations</ce:title><ce:author-group><ce:author><ce:given-name>S.G.</ce:given-name><ce:surname>Edgington</ce:surname><ce:cross-ref refid="IS985925A1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>S.K.</ce:given-name><ce:surname>Atreya</ce:surname><ce:cross-ref refid="IS985925A1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>L.M.</ce:given-name><ce:surname>Trafton</ce:surname><ce:cross-ref refid="IS985925A2"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>J.J.</ce:given-name><ce:surname>Caldwell</ce:surname><ce:cross-ref refid="IS985925A3"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>R.F.</ce:given-name><ce:surname>Beebe</ce:surname><ce:cross-ref refid="IS985925A4"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>A.A.</ce:given-name><ce:surname>Simon</ce:surname><ce:cross-ref refid="IS985925A4"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>R.A.</ce:given-name><ce:surname>West</ce:surname><ce:cross-ref refid="IS985925A5"><ce:sup>e</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>C.</ce:given-name><ce:surname>Barnet</ce:surname><ce:cross-ref refid="IS985925A6"><ce:sup>f</ce:sup></ce:cross-ref></ce:author><ce:affiliation id="IS985925A1"><ce:label>a</ce:label><ce:textfn>Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Michigan, 48109-2143</ce:textfn></ce:affiliation><ce:affiliation id="IS985925A2"><ce:label>b</ce:label><ce:textfn>McDonald Observatory, University of Texas, Austin, Texas, 78712</ce:textfn></ce:affiliation><ce:affiliation id="IS985925A3"><ce:label>c</ce:label><ce:textfn>Department of Physics and Astronomy, York University, North York, Ontario, M35 1P3, Canada</ce:textfn></ce:affiliation><ce:affiliation id="IS985925A4"><ce:label>d</ce:label><ce:textfn>Astronomy Department, New Mexico State University, Las Cruces, New Mexico, 88033</ce:textfn></ce:affiliation><ce:affiliation id="IS985925A5"><ce:label>e</ce:label><ce:textfn>Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, 91109</ce:textfn></ce:affiliation><ce:affiliation id="IS985925A6"><ce:label>f</ce:label><ce:textfn>NASA Goddard Space Flight Center, Greenbelt, Maryland, 20771</ce:textfn></ce:affiliation></ce:author-group><ce:date-received day="9" month="7" year="1997"></ce:date-received><ce:date-revised day="5" month="2" year="1998"></ce:date-revised><ce:abstract><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>Ultraviolet spectra in the spectral region from 160 to 230 nm were taken with the Hubble Space Telescope Faint Object Spectrograph in May 1992. We analyze these data to obtain the altitude distribution of ammonia and its variation with latitude from 6°N to 25°N. Ammonia condenses below the 150-mbar level, above which it departs from saturation due to photolysis. Using a photochemical model, we also derive the value of atmospheric eddy mixing coefficients at the observed latitudes. It is found that the eddy diffusion coefficient varies from 1.5 × 10<ce:sup>4</ce:sup>cm<ce:sup>2</ce:sup>s<ce:sup>−1</ce:sup>at 450 mbar to 4.9 × 10<ce:sup>2</ce:sup>cm<ce:sup>2</ce:sup>s<ce:sup>−1</ce:sup>at 120 mbar. The vertical distribution of ammonia and the eddy diffusion coefficient do not show a large variation with latitude. We also determine an acetylene mixing ratio of (10–30) × 10<ce:sup>−9</ce:sup>near 80 mbar and an upper limit of 1.5 × 10<ce:sup>−7</ce:sup>for the phosphine mixing ratio, if PH<ce:inf>3</ce:inf>is mixed uniformly below the 140 mbar level. The existence of particulate haze at low and high latitudes is also investigated.</ce:simple-para></ce:abstract-sec></ce:abstract></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>On the Latitude Variation of Ammonia, Acetylene, and Phosphine Altitude Profiles on Jupiter from HST Faint Object Spectrograph Observations</title></titleInfo><titleInfo type="alternative" lang="en" contentType="CDATA"><title>On the Latitude Variation of Ammonia, Acetylene, and Phosphine Altitude Profiles on Jupiter from HST Faint Object Spectrograph Observations</title></titleInfo><name type="personal"><namePart type="given">S.G.</namePart><namePart type="family">Edgington</namePart><affiliation>Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Michigan, 48109-2143</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.K.</namePart><namePart type="family">Atreya</namePart><affiliation>Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Michigan, 48109-2143</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.M.</namePart><namePart type="family">Trafton</namePart><affiliation>McDonald Observatory, University of Texas, Austin, Texas, 78712</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.J.</namePart><namePart type="family">Caldwell</namePart><affiliation>Department of Physics and Astronomy, York University, North York, Ontario, M35 1P3, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.F.</namePart><namePart type="family">Beebe</namePart><affiliation>Astronomy Department, New Mexico State University, Las Cruces, New Mexico, 88033</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.A.</namePart><namePart type="family">Simon</namePart><affiliation>Astronomy Department, New Mexico State University, Las Cruces, New Mexico, 88033</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.A.</namePart><namePart type="family">West</namePart><affiliation>Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, 91109</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C.</namePart><namePart type="family">Barnet</namePart><affiliation>NASA Goddard Space Flight Center, Greenbelt, Maryland, 20771</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">1998</dateIssued><dateModified encoding="w3cdtf">1998-02-05</dateModified><copyrightDate encoding="w3cdtf">1998</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">Ultraviolet spectra in the spectral region from 160 to 230 nm were taken with the Hubble Space Telescope Faint Object Spectrograph in May 1992. We analyze these data to obtain the altitude distribution of ammonia and its variation with latitude from 6°N to 25°N. Ammonia condenses below the 150-mbar level, above which it departs from saturation due to photolysis. Using a photochemical model, we also derive the value of atmospheric eddy mixing coefficients at the observed latitudes. It is found that the eddy diffusion coefficient varies from 1.5 × 104cm2s−1at 450 mbar to 4.9 × 102cm2s−1at 120 mbar. The vertical distribution of ammonia and the eddy diffusion coefficient do not show a large variation with latitude. We also determine an acetylene mixing ratio of (10–30) × 10−9near 80 mbar and an upper limit of 1.5 × 10−7for the phosphine mixing ratio, if PH3is mixed uniformly below the 140 mbar level. The existence of particulate haze at low and high latitudes is also investigated.</abstract><note>G. E. Hunt</note><note type="content">Section title: Regular Article</note><relatedItem type="host"><titleInfo><title>Icarus</title></titleInfo><titleInfo type="abbreviated"><title>YICAR</title></titleInfo><genre type="journal">journal</genre><originInfo><dateIssued encoding="w3cdtf">199806</dateIssued></originInfo><identifier type="ISSN">0019-1035</identifier><identifier type="PII">S0019-1035(00)X0044-9</identifier><part><date>199806</date><detail type="volume"><number>133</number><caption>vol.</caption></detail><detail type="issue"><number>2</number><caption>no.</caption></detail><extent unit="issue pages"><start>163</start><end>325</end></extent><extent unit="pages"><start>192</start><end>209</end></extent></part></relatedItem><identifier type="istex">5CF2D76DE67CFA0351443AF354FB9B2F0AC05D64</identifier><identifier type="DOI">10.1006/icar.1998.5925</identifier><identifier type="PII">S0019-1035(98)95925-5</identifier><accessCondition type="use and reproduction" contentType="copyright">©1998 Academic Press</accessCondition><recordInfo><recordContentSource>ELSEVIER</recordContentSource><recordOrigin>Academic Press, ©1998</recordOrigin></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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