The Hanle effect of the coronal L α line of hydrogen: Theoretical investigation
Identifieur interne : 001951 ( Istex/Corpus ); précédent : 001950; suivant : 001952The Hanle effect of the coronal L α line of hydrogen: Theoretical investigation
Auteurs : V. Bommier ; S. Sahal-BréchotSource :
- Solar Physics [ 0038-0938 ] ; 1982-05-01.
Abstract
Abstract: This paper is devoted to a computation of the effect of a magnetic field on the linear polarization of the coronal Lα line of hydrogen. Recent works (Gabriel et al., 1971) have shown that the linear polarization of this line is due to resonant scattering of the incident chromospheric Lα line. The Hanle effect is the modification of this linear polarization, due to the magnetic field. After having briefly recalled the main features of this effect and the conditions of the coronal Lα line formation, we present the theoretical formalism to be used for Hanle effect computations. The effect of the hyperfine structure of the line is included. Then the results of our computations are given in terms of linear polarization as a function of the magnetic field. We get that the effect of the hyperfine structure on these results is negligible, although this is not evident a priori. When the hyperfine structure is neglected, the line structure is simplified and the Hanle effect can be expressed with analytical formulae, which we give in the last part of this paper. After integration along the line of sight, these formulae could be used for magnetic field determination in the solar corona from measurements of the linear polarization of the Lα line.
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DOI: 10.1007/BF00151151
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ISTEX:F60B0C63CDA18A5106A2FDA247513B6F1E92F333Le document en format XML
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Sahal-Bréchot</name><affiliation><mods:affiliation>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale, Observatoire de Paris-Meudon, 92190, Meudon, France</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:F60B0C63CDA18A5106A2FDA247513B6F1E92F333</idno><date when="1982" year="1982">1982</date><idno type="doi">10.1007/BF00151151</idno><idno type="url">https://api.istex.fr/document/F60B0C63CDA18A5106A2FDA247513B6F1E92F333/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001951</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001951</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main" xml:lang="en">The Hanle effect of the coronal L α line of hydrogen: Theoretical investigation</title><author><name sortKey="Bommier, V" sort="Bommier, V" uniqKey="Bommier V" first="V." last="Bommier">V. Bommier</name><affiliation><mods:affiliation>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale, Observatoire de Paris-Meudon, 92190, Meudon, France</mods:affiliation></affiliation></author><author><name sortKey="Sahal Brechot, S" sort="Sahal Brechot, S" uniqKey="Sahal Brechot S" first="S." last="Sahal-Bréchot">S. Sahal-Bréchot</name><affiliation><mods:affiliation>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale, Observatoire de Paris-Meudon, 92190, Meudon, France</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Solar Physics</title><title level="j" type="sub">A Journal for Solar and Solar-Stellar Research and the Study of Solar Terrestrial Physics</title><title level="j" type="abbrev">Sol Phys</title><idno type="ISSN">0038-0938</idno><idno type="eISSN">1573-093X</idno><imprint><publisher>Kluwer Academic Publishers</publisher><pubPlace>Dordrecht</pubPlace><date type="published" when="1982-05-01">1982-05-01</date><biblScope unit="volume">78</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="157">157</biblScope><biblScope unit="page" to="178">178</biblScope></imprint><idno type="ISSN">0038-0938</idno></series><idno type="istex">F60B0C63CDA18A5106A2FDA247513B6F1E92F333</idno><idno type="DOI">10.1007/BF00151151</idno><idno type="ArticleID">BF00151151</idno><idno type="ArticleID">Art14</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0038-0938</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Abstract: This paper is devoted to a computation of the effect of a magnetic field on the linear polarization of the coronal Lα line of hydrogen. Recent works (Gabriel et al., 1971) have shown that the linear polarization of this line is due to resonant scattering of the incident chromospheric Lα line. The Hanle effect is the modification of this linear polarization, due to the magnetic field. After having briefly recalled the main features of this effect and the conditions of the coronal Lα line formation, we present the theoretical formalism to be used for Hanle effect computations. The effect of the hyperfine structure of the line is included. Then the results of our computations are given in terms of linear polarization as a function of the magnetic field. We get that the effect of the hyperfine structure on these results is negligible, although this is not evident a priori. When the hyperfine structure is neglected, the line structure is simplified and the Hanle effect can be expressed with analytical formulae, which we give in the last part of this paper. After integration along the line of sight, these formulae could be used for magnetic field determination in the solar corona from measurements of the linear polarization of the Lα line.</div></front></TEI><istex><corpusName>springer</corpusName><author><json:item><name>V. Bommier</name><affiliations><json:string>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale, Observatoire de Paris-Meudon, 92190, Meudon, France</json:string></affiliations></json:item><json:item><name>S. Sahal-Bréchot</name><affiliations><json:string>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale, Observatoire de Paris-Meudon, 92190, Meudon, France</json:string></affiliations></json:item></author><articleId><json:string>BF00151151</json:string><json:string>Art14</json:string></articleId><language><json:string>eng</json:string></language><originalGenre><json:string>OriginalPaper</json:string></originalGenre><abstract>Abstract: This paper is devoted to a computation of the effect of a magnetic field on the linear polarization of the coronal Lα line of hydrogen. Recent works (Gabriel et al., 1971) have shown that the linear polarization of this line is due to resonant scattering of the incident chromospheric Lα line. The Hanle effect is the modification of this linear polarization, due to the magnetic field. After having briefly recalled the main features of this effect and the conditions of the coronal Lα line formation, we present the theoretical formalism to be used for Hanle effect computations. The effect of the hyperfine structure of the line is included. Then the results of our computations are given in terms of linear polarization as a function of the magnetic field. We get that the effect of the hyperfine structure on these results is negligible, although this is not evident a priori. When the hyperfine structure is neglected, the line structure is simplified and the Hanle effect can be expressed with analytical formulae, which we give in the last part of this paper. After integration along the line of sight, these formulae could be used for magnetic field determination in the solar corona from measurements of the linear polarization of the Lα line.</abstract><qualityIndicators><score>7.532</score><pdfVersion>1.3</pdfVersion><pdfPageSize>468 x 684 pts</pdfPageSize><refBibsNative>false</refBibsNative><keywordCount>0</keywordCount><abstractCharCount>1263</abstractCharCount><pdfWordCount>8978</pdfWordCount><pdfCharCount>39712</pdfCharCount><pdfPageCount>22</pdfPageCount><abstractWordCount>211</abstractWordCount></qualityIndicators><title>The Hanle effect of the coronal L α line of hydrogen: Theoretical investigation</title><refBibs><json:item><author><json:item><name>S Bashkin</name></json:item><json:item><name>J,O Stoner</name></json:item><json:item><name> Jr</name></json:item></author><host><author></author><title>Atomic Energy Levels and Grotrian Diagrams</title><publicationDate>1975</publicationDate></host><publicationDate>1975</publicationDate></json:item><json:item><host><pages><first>924</first></pages><author><json:item><name>G,S Basri</name></json:item><json:item><name>J,L Linsky</name></json:item><json:item><name>J,D F Bartoe</name></json:item><json:item><name>G,E Brueckner</name></json:item><json:item><name>Van Hoosier</name></json:item><json:item><name>M,E </name></json:item></author><publicationDate>1979</publicationDate></host></json:item><json:item><author><json:item><name>J,M Beckers</name></json:item></author><host><volume>37</volume><pages><first>351</first></pages><author></author><title>SolarPhys</title><publicationDate>1974</publicationDate></host><publicationDate>1974</publicationDate></json:item><json:item><author><json:item><name>J,M Beckers</name></json:item><json:item><name>E Chipman</name></json:item></author><host><volume>34</volume><pages><first>151</first></pages><author></author><title>SolarPhys</title><publicationDate>1974</publicationDate></host><publicationDate>1974</publicationDate></json:item><json:item><host><author><json:item><name>V Bommier</name></json:item></author><publicationDate>1977</publicationDate></host></json:item><json:item><author><json:item><name>V Bommier</name></json:item></author><host><volume>87</volume><pages><first>109</first></pages><author></author><title>Astron. 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Neth</title><publicationDate>1950</publicationDate></host><publicationDate>1950</publicationDate></json:item><json:item><author><json:item><name>W,L Wiese</name></json:item><json:item><name>M,W Smith</name></json:item><json:item><name>B,M Glennon</name></json:item></author><host><volume>1</volume><author></author><title>Atomic Transition Probabilities</title><publicationDate>1966</publicationDate></host><publicationDate>1966</publicationDate></json:item></refBibs><genre><json:string>research-article</json:string></genre><host><volume>78</volume><pages><last>178</last><first>157</first></pages><issn><json:string>0038-0938</json:string></issn><issue>1</issue><subject><json:item><value>Astrophysics</value></json:item></subject><journalId><json:string>11207</json:string></journalId><genre><json:string>journal</json:string></genre><language><json:string>unknown</json:string></language><eissn><json:string>1573-093X</json:string></eissn><title>Solar Physics</title><publicationDate>1982</publicationDate><copyrightDate>1982</copyrightDate></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>1982</publicationDate><copyrightDate>1982</copyrightDate><doi><json:string>10.1007/BF00151151</json:string></doi><id>F60B0C63CDA18A5106A2FDA247513B6F1E92F333</id><score>0.13211583</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/F60B0C63CDA18A5106A2FDA247513B6F1E92F333/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/F60B0C63CDA18A5106A2FDA247513B6F1E92F333/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/F60B0C63CDA18A5106A2FDA247513B6F1E92F333/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main" xml:lang="en">The Hanle effect of the coronal L α line of hydrogen: Theoretical investigation</title><respStmt><resp>Références bibliographiques récupérées via GROBID</resp><name resp="ISTEX-API">ISTEX-API (INIST-CNRS)</name></respStmt><respStmt><resp>Références bibliographiques récupérées via GROBID</resp><name resp="ISTEX-API">ISTEX-API (INIST-CNRS)</name></respStmt></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Kluwer Academic Publishers</publisher><pubPlace>Dordrecht</pubPlace><availability><p>D. 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Recent works (Gabriel et al., 1971) have shown that the linear polarization of this line is due to resonant scattering of the incident chromospheric Lα line. The Hanle effect is the modification of this linear polarization, due to the magnetic field. After having briefly recalled the main features of this effect and the conditions of the coronal Lα line formation, we present the theoretical formalism to be used for Hanle effect computations. The effect of the hyperfine structure of the line is included. Then the results of our computations are given in terms of linear polarization as a function of the magnetic field. We get that the effect of the hyperfine structure on these results is negligible, although this is not evident a priori. When the hyperfine structure is neglected, the line structure is simplified and the Hanle effect can be expressed with analytical formulae, which we give in the last part of this paper. After integration along the line of sight, these formulae could be used for magnetic field determination in the solar corona from measurements of the linear polarization of the Lα line.</p></abstract><textClass><keywords scheme="Journal Subject"><list><head>Physics</head><item><term>Astrophysics</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="1981-03-12">Created</change><change when="1982-05-01">Published</change><change xml:id="refBibs-istex" who="#ISTEX-API" when="2016-11-23">References added</change><change xml:id="refBibs-istex" who="#ISTEX-API" when="2017-01-21">References added</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/F60B0C63CDA18A5106A2FDA247513B6F1E92F333/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Springer, Publisher found" wicri:toSee="no header"><istex:xmlDeclaration>version="1.0" encoding="UTF-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//Springer-Verlag//DTD A++ V2.4//EN" URI="http://devel.springer.de/A++/V2.4/DTD/A++V2.4.dtd" name="istex:docType"></istex:docType><istex:document><Publisher><PublisherInfo><PublisherName>Kluwer Academic Publishers</PublisherName><PublisherLocation>Dordrecht</PublisherLocation></PublisherInfo><Journal><JournalInfo JournalProductType="ArchiveJournal" NumberingStyle="Unnumbered"><JournalID>11207</JournalID><JournalPrintISSN>0038-0938</JournalPrintISSN><JournalElectronicISSN>1573-093X</JournalElectronicISSN><JournalTitle>Solar Physics</JournalTitle><JournalSubTitle>A Journal for Solar and Solar-Stellar Research and the Study of Solar Terrestrial Physics</JournalSubTitle><JournalAbbreviatedTitle>Sol Phys</JournalAbbreviatedTitle><JournalSubjectGroup><JournalSubject Type="Primary">Physics</JournalSubject><JournalSubject Type="Secondary">Astrophysics</JournalSubject></JournalSubjectGroup></JournalInfo><Volume><VolumeInfo VolumeType="Regular" TocLevels="0"><VolumeIDStart>78</VolumeIDStart><VolumeIDEnd>78</VolumeIDEnd><VolumeIssueCount>2</VolumeIssueCount></VolumeInfo><Issue IssueType="Regular"><IssueInfo TocLevels="0"><IssueIDStart>1</IssueIDStart><IssueIDEnd>1</IssueIDEnd><IssueArticleCount>16</IssueArticleCount><IssueHistory><CoverDate><Year>1982</Year><Month>5</Month></CoverDate></IssueHistory><IssueCopyright><CopyrightHolderName>D. Reidel Publishing Company</CopyrightHolderName><CopyrightYear>1982</CopyrightYear></IssueCopyright></IssueInfo><Article ID="Art14"><ArticleInfo Language="En" ArticleType="OriginalPaper" NumberingStyle="Unnumbered" TocLevels="0" ContainsESM="No"><ArticleID>BF00151151</ArticleID><ArticleDOI>10.1007/BF00151151</ArticleDOI><ArticleSequenceNumber>14</ArticleSequenceNumber><ArticleTitle Language="En">The Hanle effect of the coronal L<Emphasis Type="Italic">α</Emphasis> line of hydrogen: Theoretical investigation</ArticleTitle><ArticleFirstPage>157</ArticleFirstPage><ArticleLastPage>178</ArticleLastPage><ArticleHistory><RegistrationDate><Year>2004</Year><Month>6</Month><Day>21</Day></RegistrationDate><Received><Year>1981</Year><Month>3</Month><Day>12</Day></Received></ArticleHistory><ArticleCopyright><CopyrightHolderName>D. Reidel Publishing Company</CopyrightHolderName><CopyrightYear>1982</CopyrightYear></ArticleCopyright><ArticleGrants Type="Regular"><MetadataGrant Grant="OpenAccess"></MetadataGrant><AbstractGrant Grant="OpenAccess"></AbstractGrant><BodyPDFGrant Grant="Restricted"></BodyPDFGrant><BodyHTMLGrant Grant="Restricted"></BodyHTMLGrant><BibliographyGrant Grant="Restricted"></BibliographyGrant><ESMGrant Grant="Restricted"></ESMGrant></ArticleGrants><ArticleContext><JournalID>11207</JournalID><VolumeIDStart>78</VolumeIDStart><VolumeIDEnd>78</VolumeIDEnd><IssueIDStart>1</IssueIDStart><IssueIDEnd>1</IssueIDEnd></ArticleContext></ArticleInfo><ArticleHeader><AuthorGroup><Author AffiliationIDS="Aff1"><AuthorName DisplayOrder="Western"><GivenName>V.</GivenName><FamilyName>Bommier</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff1"><AuthorName DisplayOrder="Western"><GivenName>S.</GivenName><FamilyName>Sahal-Bréchot</FamilyName></AuthorName></Author><Affiliation ID="Aff1"><OrgDivision>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale</OrgDivision><OrgName>Observatoire de Paris-Meudon</OrgName><OrgAddress><Postcode>92190</Postcode><City>Meudon</City><Country>France</Country></OrgAddress></Affiliation></AuthorGroup><Abstract ID="Abs1" Language="En"><Heading>Abstract</Heading><Para>This paper is devoted to a computation of the effect of a magnetic field on the linear polarization of the coronal L<Emphasis Type="Italic">α</Emphasis> line of hydrogen. Recent works (Gabriel <Emphasis Type="Italic">et al.</Emphasis>, 1971) have shown that the linear polarization of this line is due to resonant scattering of the incident chromospheric L<Emphasis Type="Italic">α</Emphasis> line. The Hanle effect is the modification of this linear polarization, due to the magnetic field. After having briefly recalled the main features of this effect and the conditions of the coronal L<Emphasis Type="Italic">α</Emphasis> line formation, we present the theoretical formalism to be used for Hanle effect computations. The effect of the hyperfine structure of the line is included. Then the results of our computations are given in terms of linear polarization as a function of the magnetic field. We get that the effect of the hyperfine structure on these results is negligible, although this is not evident a priori. When the hyperfine structure is neglected, the line structure is simplified and the Hanle effect can be expressed with analytical formulae, which we give in the last part of this paper. After integration along the line of sight, these formulae could be used for magnetic field determination in the solar corona from measurements of the linear polarization of the L<Emphasis Type="Italic">α</Emphasis> line.</Para></Abstract><ArticleNote Type="ProofNote"><SimplePara>In Section 1 to 4 of this paper, the Hanle effect is presented as the ‘de-polarizing’ effect of a magnetic field on polarized emitted light. This is true in the case of scattering angles of about 90° or about, which is the geometry assumed in Figures 3 to 6. In fact, far from this geometry, the Hanle effect can lead in some cases to an enhancement of polarization, and it would be more general to consider the Hanle effect as a modification of the polarization, without presuming the sense of the modification. This is a question of language and does not affect the validity of all the formulae given in this paper.</SimplePara></ArticleNote></ArticleHeader><NoBody></NoBody></Article></Issue></Volume></Journal></Publisher></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>The Hanle effect of the coronal L α line of hydrogen: Theoretical investigation</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>The Hanle effect of the coronal Lα line of hydrogen: Theoretical investigation</title></titleInfo><name type="personal"><namePart type="given">V.</namePart><namePart type="family">Bommier</namePart><affiliation>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale, Observatoire de Paris-Meudon, 92190, Meudon, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Sahal-Bréchot</namePart><affiliation>Groupe de Recherches No. 24 ‘Processus atomiques et moléculaires de l'Astrophysique’, Département d'Astrophysique Fondamentale, Observatoire de Paris-Meudon, 92190, Meudon, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="research-article" displayLabel="OriginalPaper"></genre><originInfo><publisher>Kluwer Academic Publishers</publisher><place><placeTerm type="text">Dordrecht</placeTerm></place><dateCreated encoding="w3cdtf">1981-03-12</dateCreated><dateIssued encoding="w3cdtf">1982-05-01</dateIssued><copyrightDate encoding="w3cdtf">1982</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 lang="en">Abstract: This paper is devoted to a computation of the effect of a magnetic field on the linear polarization of the coronal Lα line of hydrogen. Recent works (Gabriel et al., 1971) have shown that the linear polarization of this line is due to resonant scattering of the incident chromospheric Lα line. The Hanle effect is the modification of this linear polarization, due to the magnetic field. After having briefly recalled the main features of this effect and the conditions of the coronal Lα line formation, we present the theoretical formalism to be used for Hanle effect computations. The effect of the hyperfine structure of the line is included. Then the results of our computations are given in terms of linear polarization as a function of the magnetic field. We get that the effect of the hyperfine structure on these results is negligible, although this is not evident a priori. When the hyperfine structure is neglected, the line structure is simplified and the Hanle effect can be expressed with analytical formulae, which we give in the last part of this paper. After integration along the line of sight, these formulae could be used for magnetic field determination in the solar corona from measurements of the linear polarization of the Lα line.</abstract><relatedItem type="host"><titleInfo><title>Solar Physics</title><subTitle>A Journal for Solar and Solar-Stellar Research and the Study of Solar Terrestrial Physics</subTitle></titleInfo><titleInfo type="abbreviated"><title>Sol Phys</title></titleInfo><genre type="journal" displayLabel="Archive Journal"></genre><originInfo><dateIssued encoding="w3cdtf">1982-05-01</dateIssued><copyrightDate encoding="w3cdtf">1982</copyrightDate></originInfo><subject><genre>Physics</genre><topic>Astrophysics</topic></subject><identifier type="ISSN">0038-0938</identifier><identifier type="eISSN">1573-093X</identifier><identifier type="JournalID">11207</identifier><identifier type="IssueArticleCount">16</identifier><identifier type="VolumeIssueCount">2</identifier><part><date>1982</date><detail type="volume"><number>78</number><caption>vol.</caption></detail><detail type="issue"><number>1</number><caption>no.</caption></detail><extent unit="pages"><start>157</start><end>178</end></extent></part><recordInfo><recordOrigin>D. Reidel Publishing Company, 1982</recordOrigin></recordInfo></relatedItem><identifier type="istex">F60B0C63CDA18A5106A2FDA247513B6F1E92F333</identifier><identifier type="DOI">10.1007/BF00151151</identifier><identifier type="ArticleID">BF00151151</identifier><identifier type="ArticleID">Art14</identifier><accessCondition type="use and reproduction" contentType="copyright">D. Reidel Publishing Company, 1982</accessCondition><recordInfo><recordContentSource>SPRINGER</recordContentSource><recordOrigin>D. Reidel Publishing Company, 1982</recordOrigin></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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