On the analysis of the H Lyman- α dayglow of Jupiter, Saturn and Uranus
Identifieur interne : 001421 ( Istex/Corpus ); précédent : 001420; suivant : 001422On the analysis of the H Lyman- α dayglow of Jupiter, Saturn and Uranus
Auteurs : C. Emerich ; L. Ben Jaffel ; R. PrangéSource :
- Planetary and Space Science [ 0032-0633 ] ; 1993.
Abstract
A new radiative transfer model, particularly well adapted to calculations in inhomogeneous atmospheres, has been applied, during the last 4 years, to analyse new and older Lyman-α airglow data from three giant planets. We review all the results obtained so far. Several features which were not accounted for by using the previous transfer codes have been satisfactorily simulated, using essentially the scattering of the solar and the interplanetary Lyman-α lines by hydrogen in the upper atmospheres. The search for a good fit both in intensity and in shape of the limb to limb data, and/or of the line profiles, provided constraints on the dynamics of the atmospheres, through the estimate of either the eddy diffusion coefficient, the total [H] column density, or of the possibility of some nonthermal turbulence processes at high altitude. Consequently, the need for an “electroglow” process for the Lyman-α emission was considerably reduced and may be dismissed in the majority of cases.
Url:
DOI: 10.1016/0032-0633(93)90070-I
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We review all the results obtained so far. Several features which were not accounted for by using the previous transfer codes have been satisfactorily simulated, using essentially the scattering of the solar and the interplanetary Lyman-α lines by hydrogen in the upper atmospheres. The search for a good fit both in intensity and in shape of the limb to limb data, and/or of the line profiles, provided constraints on the dynamics of the atmospheres, through the estimate of either the eddy diffusion coefficient, the total [H] column density, or of the possibility of some nonthermal turbulence processes at high altitude. Consequently, the need for an “electroglow” process for the Lyman-α emission was considerably reduced and may be dismissed in the majority of cases.</div></front></TEI><istex><corpusName>elsevier</corpusName><author><json:item><name>C. Emerich</name><affiliations><json:string>Institut d'Astrophysique Spatiale, Orsay, France</json:string></affiliations></json:item><json:item><name>L. Ben Jaffel</name><affiliations><json:string>Institut d'Astrophysique de Paris, Paris, France</json:string></affiliations></json:item><json:item><name>R. Prangé</name><affiliations><json:string>Institut d'Astrophysique Spatiale, Orsay, France</json:string></affiliations></json:item></author><language><json:string>eng</json:string></language><originalGenre><json:string>Full-length article</json:string></originalGenre><abstract>A new radiative transfer model, particularly well adapted to calculations in inhomogeneous atmospheres, has been applied, during the last 4 years, to analyse new and older Lyman-α airglow data from three giant planets. We review all the results obtained so far. Several features which were not accounted for by using the previous transfer codes have been satisfactorily simulated, using essentially the scattering of the solar and the interplanetary Lyman-α lines by hydrogen in the upper atmospheres. The search for a good fit both in intensity and in shape of the limb to limb data, and/or of the line profiles, provided constraints on the dynamics of the atmospheres, through the estimate of either the eddy diffusion coefficient, the total [H] column density, or of the possibility of some nonthermal turbulence processes at high altitude. Consequently, the need for an “electroglow” process for the Lyman-α emission was considerably reduced and may be dismissed in the majority of cases.</abstract><qualityIndicators><score>6.872</score><pdfVersion>1.2</pdfVersion><pdfPageSize>612 x 828 pts</pdfPageSize><refBibsNative>true</refBibsNative><keywordCount>0</keywordCount><abstractCharCount>992</abstractCharCount><pdfWordCount>5829</pdfWordCount><pdfCharCount>34975</pdfCharCount><pdfPageCount>9</pdfPageCount><abstractWordCount>156</abstractWordCount></qualityIndicators><title>On the analysis of the H Lyman- α dayglow of Jupiter, Saturn and Uranus</title><pii><json:string>0032-0633(93)90070-I</json:string></pii><refBibs><json:item><author><json:item><name>L. Ben Jaffel</name></json:item><json:item><name>A. Vidal-Madjar</name></json:item></author><host><volume>220</volume><pages><first>306</first></pages><author></author><title>Astron. 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J.</title></host><title>Hydrocarbon photochemistry and Lyman alpha albedo of Jupiter</title></json:item></refBibs><genre><json:string>research-article</json:string></genre><serie><pages><last>469</last><first>463</first></pages><conference><json:item><name>Proc. 3rd European IUE Conf. - Madrid</name></json:item></conference><language><json:string>unknown</json:string></language><title>Proc. 3rd European IUE Conf.</title></serie><host><volume>41</volume><pii><json:string>S0032-0633(00)X0333-9</json:string></pii><pages><last>371</last><first>363</first></pages><issn><json:string>0032-0633</json:string></issn><issue>5</issue><genre><json:string>journal</json:string></genre><language><json:string>unknown</json:string></language><title>Planetary and Space Science</title><publicationDate>1993</publicationDate></host><categories><wos><json:string>science</json:string><json:string>astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>natural sciences</json:string><json:string>physics & astronomy</json:string><json:string>astronomy & astrophysics</json:string></scienceMetrix></categories><publicationDate>1993</publicationDate><copyrightDate>1993</copyrightDate><doi><json:string>10.1016/0032-0633(93)90070-I</json:string></doi><id>35952E1B65004624AFCBD308D9FCA4352C20EF05</id><score>0.20938945</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/35952E1B65004624AFCBD308D9FCA4352C20EF05/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/35952E1B65004624AFCBD308D9FCA4352C20EF05/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/35952E1B65004624AFCBD308D9FCA4352C20EF05/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a">On the analysis of the H Lyman- α dayglow of Jupiter, Saturn and Uranus</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>ELSEVIER</publisher><availability><p>ELSEVIER</p></availability><date>1993</date></publicationStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a">On the analysis of the H Lyman- α dayglow of Jupiter, Saturn and Uranus</title><author xml:id="author-1"><persName><forename type="first">C.</forename><surname>Emerich</surname></persName><note type="correspondence"><p>Correspondence to: C. Emerich.</p></note><affiliation>Institut d'Astrophysique Spatiale, Orsay, France</affiliation></author><author xml:id="author-2"><persName><forename type="first">L.</forename><surname>Ben Jaffel</surname></persName><affiliation>Institut d'Astrophysique de Paris, Paris, France</affiliation></author><author xml:id="author-3"><persName><forename type="first">R.</forename><surname>Prangé</surname></persName><affiliation>Institut d'Astrophysique Spatiale, Orsay, France</affiliation></author></analytic><monogr><title level="j">Planetary and Space Science</title><title level="j" type="abbrev">PSS</title><idno type="pISSN">0032-0633</idno><idno type="PII">S0032-0633(00)X0333-9</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1993"></date><biblScope unit="volume">41</biblScope><biblScope unit="issue">5</biblScope><biblScope unit="page" from="363">363</biblScope><biblScope unit="page" to="371">371</biblScope></imprint></monogr><idno type="istex">35952E1B65004624AFCBD308D9FCA4352C20EF05</idno><idno type="DOI">10.1016/0032-0633(93)90070-I</idno><idno type="PII">0032-0633(93)90070-I</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>1993</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>A new radiative transfer model, particularly well adapted to calculations in inhomogeneous atmospheres, has been applied, during the last 4 years, to analyse new and older Lyman-α airglow data from three giant planets. We review all the results obtained so far. Several features which were not accounted for by using the previous transfer codes have been satisfactorily simulated, using essentially the scattering of the solar and the interplanetary Lyman-α lines by hydrogen in the upper atmospheres. The search for a good fit both in intensity and in shape of the limb to limb data, and/or of the line profiles, provided constraints on the dynamics of the atmospheres, through the estimate of either the eddy diffusion coefficient, the total [H] column density, or of the possibility of some nonthermal turbulence processes at high altitude. Consequently, the need for an “electroglow” process for the Lyman-α emission was considerably reduced and may be dismissed in the majority of cases.</p></abstract></profileDesc><revisionDesc><change when="1993-03-03">Modified</change><change when="1993">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/35952E1B65004624AFCBD308D9FCA4352C20EF05/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"><item-info><jid>PSS</jid><aid>9390070I</aid><ce:pii>0032-0633(93)90070-I</ce:pii><ce:doi>10.1016/0032-0633(93)90070-I</ce:doi><ce:copyright type="unknown" year="1993"></ce:copyright></item-info><head><ce:title>On the analysis of the H Lyman-<ce:italic>α</ce:italic> dayglow of Jupiter, Saturn and Uranus</ce:title><ce:author-group><ce:author><ce:given-name>C.</ce:given-name><ce:surname>Emerich</ce:surname><ce:cross-ref refid="COR1"><ce:sup>∗</ce:sup></ce:cross-ref><ce:cross-ref refid="AFF1"><ce:sup>1</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>L.</ce:given-name><ce:surname>Ben Jaffel</ce:surname><ce:cross-ref refid="AFF2"><ce:sup>2</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>R.</ce:given-name><ce:surname>Prangé</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>1</ce:sup></ce:cross-ref></ce:author><ce:affiliation id="AFF1"><ce:label>1</ce:label><ce:textfn>Institut d'Astrophysique Spatiale, Orsay, France</ce:textfn></ce:affiliation><ce:affiliation id="AFF2"><ce:label>2</ce:label><ce:textfn>Institut d'Astrophysique de Paris, Paris, France</ce:textfn></ce:affiliation><ce:correspondence id="COR1"><ce:label>∗</ce:label><ce:text>Correspondence to: C. Emerich.</ce:text></ce:correspondence></ce:author-group><ce:date-received day="19" month="11" year="1992"></ce:date-received><ce:date-revised day="3" month="3" year="1993"></ce:date-revised><ce:date-accepted day="31" month="3" year="1993"></ce:date-accepted><ce:abstract><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>A new radiative transfer model, particularly well adapted to calculations in inhomogeneous atmospheres, has been applied, during the last 4 years, to analyse new and older Lyman-<ce:italic>α</ce:italic> airglow data from three giant planets. We review all the results obtained so far. Several features which were not accounted for by using the previous transfer codes have been satisfactorily simulated, using essentially the scattering of the solar and the interplanetary Lyman-<ce:italic>α</ce:italic> lines by hydrogen in the upper atmospheres. The search for a good fit both in intensity and in shape of the limb to limb data, and/or of the line profiles, provided constraints on the dynamics of the atmospheres, through the estimate of either the eddy diffusion coefficient, the total [H] column density, or of the possibility of some nonthermal turbulence processes at high altitude. Consequently, the need for an “electroglow” process for the Lyman-<ce:italic>α</ce:italic> emission was considerably reduced and may be dismissed in the majority of cases.</ce:simple-para></ce:abstract-sec></ce:abstract></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo><title>On the analysis of the H Lyman- α dayglow of Jupiter, Saturn and Uranus</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>On the analysis of the H Lyman-</title></titleInfo><name type="personal"><namePart type="given">C.</namePart><namePart type="family">Emerich</namePart><affiliation>Institut d'Astrophysique Spatiale, Orsay, France</affiliation><description>Correspondence to: C. Emerich.</description><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.</namePart><namePart type="family">Ben Jaffel</namePart><affiliation>Institut d'Astrophysique de Paris, Paris, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Prangé</namePart><affiliation>Institut d'Astrophysique Spatiale, Orsay, France</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">1993</dateIssued><dateModified encoding="w3cdtf">1993-03-03</dateModified><copyrightDate encoding="w3cdtf">1993</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">A new radiative transfer model, particularly well adapted to calculations in inhomogeneous atmospheres, has been applied, during the last 4 years, to analyse new and older Lyman-α airglow data from three giant planets. We review all the results obtained so far. Several features which were not accounted for by using the previous transfer codes have been satisfactorily simulated, using essentially the scattering of the solar and the interplanetary Lyman-α lines by hydrogen in the upper atmospheres. The search for a good fit both in intensity and in shape of the limb to limb data, and/or of the line profiles, provided constraints on the dynamics of the atmospheres, through the estimate of either the eddy diffusion coefficient, the total [H] column density, or of the possibility of some nonthermal turbulence processes at high altitude. Consequently, the need for an “electroglow” process for the Lyman-α emission was considerably reduced and may be dismissed in the majority of cases.</abstract><relatedItem type="host"><titleInfo><title>Planetary and Space Science</title></titleInfo><titleInfo type="abbreviated"><title>PSS</title></titleInfo><genre type="journal">journal</genre><originInfo><dateIssued encoding="w3cdtf">199305</dateIssued></originInfo><identifier type="ISSN">0032-0633</identifier><identifier type="PII">S0032-0633(00)X0333-9</identifier><part><date>199305</date><detail type="volume"><number>41</number><caption>vol.</caption></detail><detail type="issue"><number>5</number><caption>no.</caption></detail><extent unit="issue pages"><start>333</start><end>408</end></extent><extent unit="pages"><start>363</start><end>371</end></extent></part></relatedItem><identifier type="istex">35952E1B65004624AFCBD308D9FCA4352C20EF05</identifier><identifier type="DOI">10.1016/0032-0633(93)90070-I</identifier><identifier type="PII">0032-0633(93)90070-I</identifier><recordInfo><recordContentSource>ELSEVIER</recordContentSource></recordInfo></mods></metadata></istex></record>Pour manipuler ce document sous Unix (Dilib)
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