Voyager 2 photopolarimeter observations of Titan
Identifieur interne : 001D67 ( Istex/Corpus ); précédent : 001D66; suivant : 001D68Voyager 2 photopolarimeter observations of Titan
Auteurs : R. A. West ; A. L. Lane ; H. Hart ; K. E. Simmons ; C. W. Hord ; D. L. Coffeen ; L. W. Esposito ; M. Sato ; R. B. PomphreySource :
- Journal of Geophysical Research: Space Physics [ 0148-0227 ] ; 1983-11-01.
Abstract
Observations of Titan's whole disk polarization at 2460 and 7500 Å are presented and analyzed in terms of model scattering atmospheres. If the Titan aerosols are spherical or nearly spherical, no single combination of refractive index and size distribution is able to fit data at both wavelengths. However, a vertically inhomogeneous distribution suggested by Tomasko and Smith (1980), characterized by a size gradient with altitude, fits the data at 2640 Å moderately well but must be modified at intermediate and large optical depths to fit the 7500‐Å data. Results for synthetic phase functions indicate that the single scattering polarization must be 70% or larger in the UV and 78% or larger in the near‐IR at 90° phase angle, depending on the phase function. If the correct phase function is similar to that for 0.5‐μm‐radius spheres, the UV single‐scattered polarization must be 84% and the near‐IR single‐scattered polarization must be over 90%. Such large polarizations are impossible for 0.5‐μm‐radius spheres but may be possible for nonspherical particles with effective radii near 0.5 µm, although the existence of nonspherical particles with the scattering properties required by these and other observations has not been demonstrated.
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DOI: 10.1029/JA088iA11p08699
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Pomphrey</name></author></analytic><monogr></monogr><series><title level="j">Journal of Geophysical Research: Space Physics</title><title level="j" type="abbrev">J. Geophys. Res.</title><idno type="ISSN">0148-0227</idno><idno type="eISSN">2156-2202</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><date type="published" when="1983-11-01">1983-11-01</date><biblScope unit="volume">88</biblScope><biblScope unit="issue">A11</biblScope><biblScope unit="page" from="8699">8699</biblScope><biblScope unit="page" to="8708">8708</biblScope></imprint><idno type="ISSN">0148-0227</idno></series><idno type="istex">E6E43C5796B037F763772D728132DEBC37DC3A29</idno><idno type="DOI">10.1029/JA088iA11p08699</idno><idno type="ArticleID">3C0560</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">Observations of Titan's whole disk polarization at 2460 and 7500 Å are presented and analyzed in terms of model scattering atmospheres. If the Titan aerosols are spherical or nearly spherical, no single combination of refractive index and size distribution is able to fit data at both wavelengths. However, a vertically inhomogeneous distribution suggested by Tomasko and Smith (1980), characterized by a size gradient with altitude, fits the data at 2640 Å moderately well but must be modified at intermediate and large optical depths to fit the 7500‐Å data. Results for synthetic phase functions indicate that the single scattering polarization must be 70% or larger in the UV and 78% or larger in the near‐IR at 90° phase angle, depending on the phase function. If the correct phase function is similar to that for 0.5‐μm‐radius spheres, the UV single‐scattered polarization must be 84% and the near‐IR single‐scattered polarization must be over 90%. Such large polarizations are impossible for 0.5‐μm‐radius spheres but may be possible for nonspherical particles with effective radii near 0.5 µm, although the existence of nonspherical particles with the scattering properties required by these and other observations has not been demonstrated.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>R. A. West</name></json:item><json:item><name>A. L. Lane</name></json:item><json:item><name>H. Hart</name></json:item><json:item><name>K. E. Simmons</name></json:item><json:item><name>C. W. Hord</name></json:item><json:item><name>D. L. Coffeen</name></json:item><json:item><name>L. W. Esposito</name></json:item><json:item><name>M. Sato</name></json:item><json:item><name>R. B. Pomphrey</name></json:item></author><articleId><json:string>3C0560</json:string></articleId><language><json:string>eng</json:string></language><abstract>Observations of Titan's whole disk polarization at 2460 and 7500 Å are presented and analyzed in terms of model scattering atmospheres. If the Titan aerosols are spherical or nearly spherical, no single combination of refractive index and size distribution is able to fit data at both wavelengths. However, a vertically inhomogeneous distribution suggested by Tomasko and Smith (1980), characterized by a size gradient with altitude, fits the data at 2640 Å moderately well but must be modified at intermediate and large optical depths to fit the 7500‐Å data. Results for synthetic phase functions indicate that the single scattering polarization must be 70% or larger in the UV and 78% or larger in the near‐IR at 90° phase angle, depending on the phase function. If the correct phase function is similar to that for 0.5‐μm‐radius spheres, the UV single‐scattered polarization must be 84% and the near‐IR single‐scattered polarization must be over 90%. Such large polarizations are impossible for 0.5‐μm‐radius spheres but may be possible for nonspherical particles with effective radii near 0.5 µm, although the existence of nonspherical particles with the scattering properties required by these and other observations has not been demonstrated.</abstract><qualityIndicators><score>5.531</score><pdfVersion>1.3</pdfVersion><pdfPageSize>604 x 806 pts</pdfPageSize><refBibsNative>true</refBibsNative><keywordCount>0</keywordCount><abstractCharCount>1248</abstractCharCount><pdfWordCount>3227</pdfWordCount><pdfCharCount>31815</pdfCharCount><pdfPageCount>10</pdfPageCount><abstractWordCount>192</abstractWordCount></qualityIndicators><title>Voyager 2 photopolarimeter observations of Titan</title><genre.original><json:string>article</json:string></genre.original><genre><json:string>article</json:string></genre><host><volume>88</volume><publisherId><json:string>JGRA</json:string></publisherId><pages><total>10</total><last>8708</last><first>8699</first></pages><issn><json:string>0148-0227</json:string></issn><issue>A11</issue><subject><json:item><value>Voyager Mission to Saturn Color Plates</value></json:item></subject><genre><json:string>journal</json:string></genre><language><json:string>unknown</json:string></language><eissn><json:string>2156-2202</json:string></eissn><title>Journal of Geophysical Research: Space Physics</title><doi><json:string>10.1002/(ISSN)2156-2202a</json:string></doi></host><publicationDate>1983</publicationDate><copyrightDate>1983</copyrightDate><doi><json:string>10.1029/JA088iA11p08699</json:string></doi><id>E6E43C5796B037F763772D728132DEBC37DC3A29</id><fulltext><json:item><original>true</original><mimetype>application/pdf</mimetype><extension>pdf</extension><uri>https://api.istex.fr/document/E6E43C5796B037F763772D728132DEBC37DC3A29/fulltext/pdf</uri></json:item><json:item><original>false</original><mimetype>application/zip</mimetype><extension>zip</extension><uri>https://api.istex.fr/document/E6E43C5796B037F763772D728132DEBC37DC3A29/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/E6E43C5796B037F763772D728132DEBC37DC3A29/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main" xml:lang="en">Voyager 2 photopolarimeter observations of Titan</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><availability><p>WILEY</p></availability><date>1983</date></publicationStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">Voyager 2 photopolarimeter observations of Titan</title><author><persName><forename type="first">R. A.</forename><surname>West</surname></persName></author><author><persName><forename type="first">A. L.</forename><surname>Lane</surname></persName></author><author><persName><forename type="first">H.</forename><surname>Hart</surname></persName></author><author><persName><forename type="first">K. E.</forename><surname>Simmons</surname></persName></author><author><persName><forename type="first">C. W.</forename><surname>Hord</surname></persName></author><author><persName><forename type="first">D. L.</forename><surname>Coffeen</surname></persName></author><author><persName><forename type="first">L. W.</forename><surname>Esposito</surname></persName></author><author><persName><forename type="first">M.</forename><surname>Sato</surname></persName></author><author><persName><forename type="first">R. B.</forename><surname>Pomphrey</surname></persName></author></analytic><monogr><title level="j">Journal of Geophysical Research: Space Physics</title><title level="j" type="abbrev">J. Geophys. 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If the Titan aerosols are spherical or nearly spherical, no single combination of refractive index and size distribution is able to fit data at both wavelengths. However, a vertically inhomogeneous distribution suggested by Tomasko and Smith (1980), characterized by a size gradient with altitude, fits the data at 2640 Å moderately well but must be modified at intermediate and large optical depths to fit the 7500‐Å data. Results for synthetic phase functions indicate that the single scattering polarization must be 70% or larger in the UV and 78% or larger in the near‐IR at 90° phase angle, depending on the phase function. If the correct phase function is similar to that for 0.5‐μm‐radius spheres, the UV single‐scattered polarization must be 84% and the near‐IR single‐scattered polarization must be over 90%. Such large polarizations are impossible for 0.5‐μm‐radius spheres but may be possible for nonspherical particles with effective radii near 0.5 µm, although the existence of nonspherical particles with the scattering properties required by these and other observations has not been demonstrated.</p></abstract><textClass><keywords scheme="Journal Subject"><list><head>article-category</head><item><term>Voyager Mission to Saturn Color Plates</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="1982-10-07">Received</change><change when="1983-04-04">Registration</change><change when="1983-11-01">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/E6E43C5796B037F763772D728132DEBC37DC3A29/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="jgra6765"><header><publicationMeta level="product"><doi>10.1002/(ISSN)2156-2202a</doi><issn type="print">0148-0227</issn><issn type="electronic">2156-2202</issn><idGroup><id type="product" value="JGRA"></id><id type="coden" value="JGREA2"></id></idGroup><titleGroup><title type="main" xml:lang="en" sort="JOURNAL OF GEOPHYSICAL RESEARCH: SPACE PHYSICS">Journal of Geophysical Research: Space Physics</title><title type="short">J. 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A.</givenNames></author>, <author><givenNames>A. L.</givenNames> <familyName>Lane</familyName></author>, <author><givenNames>H.</givenNames> <familyName>Hart</familyName></author>, <author><givenNames>K. E.</givenNames> <familyName>Simmons</familyName></author>, <author><givenNames>C. W.</givenNames> <familyName>Hord</familyName></author>, <author><givenNames>D. L.</givenNames> <familyName>Coffeen</familyName></author>, <author><givenNames>L. W.</givenNames> <familyName>Esposito</familyName></author>, <author><givenNames>M.</givenNames> <familyName>Sato</familyName></author>, and <author><givenNames>R. B.</givenNames> <familyName>Pomphrey</familyName></author> (<pubYear year="1983">1983</pubYear>), <articleTitle>Voyager 2 photopolarimeter observations of Titan</articleTitle>, <journalTitle>J. Geophys. Res.</journalTitle>, <vol>88</vol>(<issue>A11</issue>), <pageFirst>8699</pageFirst>–<pageLast>8708</pageLast>, doi:<accessionId ref="info:doi/10.1029/JA088iA11p08699">10.1029/JA088iA11p08699</accessionId>.</citation></selfCitationGroup><linkGroup><link type="toTypesetVersion" href="file:JGRA.JGRA6765.pdf"></link></linkGroup></publicationMeta><contentMeta><titleGroup><title type="main">Voyager 2 photopolarimeter observations of Titan</title><title type="shortAuthors">West ET AL.</title></titleGroup><creators><creator xml:id="jgra6765-cr-0001"><personName><givenNames>R. A.</givenNames><familyName>West</familyName></personName></creator><creator xml:id="jgra6765-cr-0002"><personName><givenNames>A. L.</givenNames><familyName>Lane</familyName></personName></creator><creator xml:id="jgra6765-cr-0003"><personName><givenNames>H.</givenNames><familyName>Hart</familyName></personName></creator><creator xml:id="jgra6765-cr-0004"><personName><givenNames>K. E.</givenNames><familyName>Simmons</familyName></personName></creator><creator xml:id="jgra6765-cr-0005"><personName><givenNames>C. W.</givenNames><familyName>Hord</familyName></personName></creator><creator xml:id="jgra6765-cr-0006"><personName><givenNames>D. L.</givenNames><familyName>Coffeen</familyName></personName></creator><creator xml:id="jgra6765-cr-0007"><personName><givenNames>L. W.</givenNames><familyName>Esposito</familyName></personName></creator><creator xml:id="jgra6765-cr-0008"><personName><givenNames>M.</givenNames><familyName>Sato</familyName></personName></creator><creator xml:id="jgra6765-cr-0009"><personName><givenNames>R. B.</givenNames><familyName>Pomphrey</familyName></personName></creator></creators><abstractGroup><abstract type="main"><p xml:id="jgra6765-para-0001">Observations of Titan's whole disk polarization at 2460 and 7500 Å are presented and analyzed in terms of model scattering atmospheres. If the Titan aerosols are spherical or nearly spherical, no single combination of refractive index and size distribution is able to fit data at both wavelengths. However, a vertically inhomogeneous distribution suggested by Tomasko and Smith (1980), characterized by a size gradient with altitude, fits the data at 2640 Å moderately well but must be modified at intermediate and large optical depths to fit the 7500‐Å data. Results for synthetic phase functions indicate that the single scattering polarization must be 70% or larger in the UV and 78% or larger in the near‐IR at 90° phase angle, depending on the phase function. If the correct phase function is similar to that for 0.5‐μm‐radius spheres, the UV single‐scattered polarization must be 84% and the near‐IR single‐scattered polarization must be over 90%. Such large polarizations are impossible for 0.5‐μm‐radius spheres but may be possible for nonspherical particles with effective radii near 0.5 µm, although the existence of nonspherical particles with the scattering properties required by these and other observations has not been demonstrated.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Voyager 2 photopolarimeter observations of Titan</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Voyager 2 photopolarimeter observations of Titan</title></titleInfo><name type="personal"><namePart type="given">R. A.</namePart><namePart type="family">West</namePart></name><name type="personal"><namePart type="given">A. L.</namePart><namePart type="family">Lane</namePart></name><name type="personal"><namePart type="given">H.</namePart><namePart type="family">Hart</namePart></name><name type="personal"><namePart type="given">K. E.</namePart><namePart type="family">Simmons</namePart></name><name type="personal"><namePart type="given">C. W.</namePart><namePart type="family">Hord</namePart></name><name type="personal"><namePart type="given">D. L.</namePart><namePart type="family">Coffeen</namePart></name><name type="personal"><namePart type="given">L. W.</namePart><namePart type="family">Esposito</namePart></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Sato</namePart></name><name type="personal"><namePart type="given">R. B.</namePart><namePart type="family">Pomphrey</namePart></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><dateIssued encoding="w3cdtf">1983-11-01</dateIssued><dateCaptured encoding="w3cdtf">1982-10-07</dateCaptured><dateValid encoding="w3cdtf">1983-04-04</dateValid><edition>West, R. A., A. L. Lane, H. Hart, K. E. Simmons, C. W. Hord, D. L. Coffeen, L. W. Esposito, M. Sato, and R. B. Pomphrey (1983), Voyager 2 photopolarimeter observations of Titan, J. Geophys. Res., 88(A11), 8699–8708, doi:10.1029/JA088iA11p08699.</edition><copyrightDate encoding="w3cdtf">1983</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType></physicalDescription><abstract>Observations of Titan's whole disk polarization at 2460 and 7500 Å are presented and analyzed in terms of model scattering atmospheres. If the Titan aerosols are spherical or nearly spherical, no single combination of refractive index and size distribution is able to fit data at both wavelengths. However, a vertically inhomogeneous distribution suggested by Tomasko and Smith (1980), characterized by a size gradient with altitude, fits the data at 2640 Å moderately well but must be modified at intermediate and large optical depths to fit the 7500‐Å data. Results for synthetic phase functions indicate that the single scattering polarization must be 70% or larger in the UV and 78% or larger in the near‐IR at 90° phase angle, depending on the phase function. If the correct phase function is similar to that for 0.5‐μm‐radius spheres, the UV single‐scattered polarization must be 84% and the near‐IR single‐scattered polarization must be over 90%. Such large polarizations are impossible for 0.5‐μm‐radius spheres but may be possible for nonspherical particles with effective radii near 0.5 µm, although the existence of nonspherical particles with the scattering properties required by these and other observations has not been demonstrated.</abstract><relatedItem type="host"><titleInfo><title>Journal of Geophysical Research: Space Physics</title></titleInfo><titleInfo type="abbreviated"><title>J. Geophys. Res.</title></titleInfo><genre type="journal">journal</genre><subject><genre>article-category</genre><topic>Voyager Mission to Saturn Color Plates</topic></subject><identifier type="ISSN">0148-0227</identifier><identifier type="eISSN">2156-2202</identifier><identifier type="DOI">10.1002/(ISSN)2156-2202a</identifier><identifier type="CODEN">JGREA2</identifier><identifier type="PublisherID">JGRA</identifier><part><date>1983</date><detail type="volume"><caption>vol.</caption><number>88</number></detail><detail type="issue"><caption>no.</caption><number>A11</number></detail><extent unit="pages"><start>8699</start><end>8708</end><total>10</total></extent></part></relatedItem><identifier type="istex">E6E43C5796B037F763772D728132DEBC37DC3A29</identifier><identifier type="DOI">10.1029/JA088iA11p08699</identifier><identifier type="ArticleID">3C0560</identifier><accessCondition type="use and reproduction" contentType="copyright">Copyright 1983 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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|texte= Voyager 2 photopolarimeter observations of Titan
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