The solar corona from SOHO
Identifieur interne : 001836 ( Istex/Corpus ); précédent : 001835; suivant : 001837The solar corona from SOHO
Auteurs : J.-C. VialSource :
- Advances in Space Research [ 0273-1177 ] ; 1993.
Abstract
The heating of the solar corona and the acceleration of the solar wind are, after decades of observations and modelling, still open questions. Many processes are possible in regions of strong magnetic field, such as waves, currents, or impulsive events which involve particles acceleration. However, no conclusion has been reached up to now. The situation is no better in open field regions where a (quiet) corona also exists and the wind is faster. Apart from a theoretical effort, a coherent diagnostic of the relevant physical quantities such as densities, temperatures, velocities and their temporal and spatial variations, is necessary. We show how the coronal package on SOHO can provide the temperature and height coverage adequate to understand both small and large scale, closed and open field, solar structures. We give examples of observing programs which address some important physical problems. Finally, we emphasize the increase of scientific return if the SOHO instrumentation is considered as a unique package.
Url:
DOI: 10.1016/0273-1177(94)90181-3
Links to Exploration step
ISTEX:3776E4854B29AD2ED75E0CC816696BBECA7F0424Le document en format XML
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Vial</name><affiliation><mods:affiliation>Institut d'Astrophysique Spatiale, Bâtiment 121, Université Paris XI, 91405 Orsay Cedex, France</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Advances in Space Research</title><title level="j" type="abbrev">JASR</title><idno type="ISSN">0273-1177</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1993">1993</date><biblScope unit="volume">14</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="181">181</biblScope><biblScope unit="page" to="194">194</biblScope></imprint><idno type="ISSN">0273-1177</idno></series><idno type="istex">3776E4854B29AD2ED75E0CC816696BBECA7F0424</idno><idno type="DOI">10.1016/0273-1177(94)90181-3</idno><idno type="PII">0273-1177(94)90181-3</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0273-1177</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The heating of the solar corona and the acceleration of the solar wind are, after decades of observations and modelling, still open questions. Many processes are possible in regions of strong magnetic field, such as waves, currents, or impulsive events which involve particles acceleration. However, no conclusion has been reached up to now. The situation is no better in open field regions where a (quiet) corona also exists and the wind is faster. Apart from a theoretical effort, a coherent diagnostic of the relevant physical quantities such as densities, temperatures, velocities and their temporal and spatial variations, is necessary. We show how the coronal package on SOHO can provide the temperature and height coverage adequate to understand both small and large scale, closed and open field, solar structures. We give examples of observing programs which address some important physical problems. Finally, we emphasize the increase of scientific return if the SOHO instrumentation is considered as a unique package.</div></front></TEI><istex><corpusName>elsevier</corpusName><author><json:item><name>J.-C. Vial</name><affiliations><json:string>Institut d'Astrophysique Spatiale, Bâtiment 121, Université Paris XI, 91405 Orsay Cedex, France</json:string></affiliations></json:item></author><language><json:string>eng</json:string></language><originalGenre><json:string>Full-length article</json:string></originalGenre><abstract>The heating of the solar corona and the acceleration of the solar wind are, after decades of observations and modelling, still open questions. Many processes are possible in regions of strong magnetic field, such as waves, currents, or impulsive events which involve particles acceleration. However, no conclusion has been reached up to now. The situation is no better in open field regions where a (quiet) corona also exists and the wind is faster. Apart from a theoretical effort, a coherent diagnostic of the relevant physical quantities such as densities, temperatures, velocities and their temporal and spatial variations, is necessary. We show how the coronal package on SOHO can provide the temperature and height coverage adequate to understand both small and large scale, closed and open field, solar structures. We give examples of observing programs which address some important physical problems. Finally, we emphasize the increase of scientific return if the SOHO instrumentation is considered as a unique package.</abstract><qualityIndicators><score>7.396</score><pdfVersion>1.4</pdfVersion><pdfPageSize>548 x 785 pts</pdfPageSize><refBibsNative>true</refBibsNative><keywordCount>0</keywordCount><abstractCharCount>1027</abstractCharCount><pdfWordCount>9518</pdfWordCount><pdfCharCount>51103</pdfCharCount><pdfPageCount>14</pdfPageCount><abstractWordCount>158</abstractWordCount></qualityIndicators><title>The solar corona from SOHO</title><pii><json:string>0273-1177(94)90181-3</json:string></pii><refBibs><json:item><author><json:item><name>G.L. Withbroe</name></json:item><json:item><name>R.W. 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Kohl</name></json:item></author><host><author></author><title>CFA Report</title></host><title>The UVCS for SOHO</title></json:item></refBibs><genre><json:string>research-article</json:string></genre><serie><pages><first>43</first></pages><language><json:string>unknown</json:string></language><title>The SOHO Mission</title></serie><host><volume>14</volume><pii><json:string>S0273-1177(00)X0309-2</json:string></pii><pages><last>194</last><first>181</first></pages><issn><json:string>0273-1177</json:string></issn><issue>4</issue><genre><json:string>journal</json:string></genre><language><json:string>unknown</json:string></language><title>Advances in Space Research</title><publicationDate>1994</publicationDate></host><publicationDate>1993</publicationDate><copyrightDate>1993</copyrightDate><doi><json:string>10.1016/0273-1177(94)90181-3</json:string></doi><id>3776E4854B29AD2ED75E0CC816696BBECA7F0424</id><score>0.1295834</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/3776E4854B29AD2ED75E0CC816696BBECA7F0424/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/3776E4854B29AD2ED75E0CC816696BBECA7F0424/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/3776E4854B29AD2ED75E0CC816696BBECA7F0424/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a">The solar corona from SOHO</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">The solar corona from SOHO</title><author xml:id="author-1"><persName><forename type="first">J.-C.</forename><surname>Vial</surname></persName><affiliation>Institut d'Astrophysique Spatiale, Bâtiment 121, Université Paris XI, 91405 Orsay Cedex, France</affiliation></author></analytic><monogr><title level="j">Advances in Space Research</title><title level="j" type="abbrev">JASR</title><idno type="pISSN">0273-1177</idno><idno type="PII">S0273-1177(00)X0309-2</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1993"></date><biblScope unit="volume">14</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="181">181</biblScope><biblScope unit="page" to="194">194</biblScope></imprint></monogr><idno type="istex">3776E4854B29AD2ED75E0CC816696BBECA7F0424</idno><idno type="DOI">10.1016/0273-1177(94)90181-3</idno><idno type="PII">0273-1177(94)90181-3</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>1993</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>The heating of the solar corona and the acceleration of the solar wind are, after decades of observations and modelling, still open questions. Many processes are possible in regions of strong magnetic field, such as waves, currents, or impulsive events which involve particles acceleration. However, no conclusion has been reached up to now. The situation is no better in open field regions where a (quiet) corona also exists and the wind is faster. Apart from a theoretical effort, a coherent diagnostic of the relevant physical quantities such as densities, temperatures, velocities and their temporal and spatial variations, is necessary. We show how the coronal package on SOHO can provide the temperature and height coverage adequate to understand both small and large scale, closed and open field, solar structures. We give examples of observing programs which address some important physical problems. Finally, we emphasize the increase of scientific return if the SOHO instrumentation is considered as a unique package.</p></abstract></profileDesc><revisionDesc><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/3776E4854B29AD2ED75E0CC816696BBECA7F0424/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>JASR</jid><aid>94901813</aid><ce:pii>0273-1177(94)90181-3</ce:pii><ce:doi>10.1016/0273-1177(94)90181-3</ce:doi><ce:copyright type="unknown" year="1993"></ce:copyright></item-info><head><ce:title>The solar corona from SOHO</ce:title><ce:author-group><ce:author><ce:given-name>J.-C.</ce:given-name><ce:surname>Vial</ce:surname></ce:author><ce:affiliation><ce:textfn>Institut d'Astrophysique Spatiale, Bâtiment 121, Université Paris XI, 91405 Orsay Cedex, France</ce:textfn></ce:affiliation></ce:author-group><ce:abstract><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>The heating of the solar corona and the acceleration of the solar wind are, after decades of observations and modelling, still open questions. Many processes are possible in regions of strong magnetic field, such as waves, currents, or impulsive events which involve particles acceleration. However, no conclusion has been reached up to now. The situation is no better in open field regions where a (quiet) corona also exists and the wind is faster. Apart from a theoretical effort, a coherent diagnostic of the relevant physical quantities such as densities, temperatures, velocities and their temporal and spatial variations, is necessary. We show how the coronal package on SOHO can provide the temperature and height coverage adequate to understand both small and large scale, closed and open field, solar structures. We give examples of observing programs which address some important physical problems. Finally, we emphasize the increase of scientific return if the SOHO instrumentation is considered as a unique package.</ce:simple-para></ce:abstract-sec></ce:abstract></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo><title>The solar corona from SOHO</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>The solar corona from SOHO</title></titleInfo><name type="personal"><namePart type="given">J.-C.</namePart><namePart type="family">Vial</namePart><affiliation>Institut d'Astrophysique Spatiale, Bâtiment 121, Université Paris XI, 91405 Orsay Cedex, 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><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">The heating of the solar corona and the acceleration of the solar wind are, after decades of observations and modelling, still open questions. Many processes are possible in regions of strong magnetic field, such as waves, currents, or impulsive events which involve particles acceleration. However, no conclusion has been reached up to now. The situation is no better in open field regions where a (quiet) corona also exists and the wind is faster. Apart from a theoretical effort, a coherent diagnostic of the relevant physical quantities such as densities, temperatures, velocities and their temporal and spatial variations, is necessary. We show how the coronal package on SOHO can provide the temperature and height coverage adequate to understand both small and large scale, closed and open field, solar structures. We give examples of observing programs which address some important physical problems. Finally, we emphasize the increase of scientific return if the SOHO instrumentation is considered as a unique package.</abstract><relatedItem type="host"><titleInfo><title>Advances in Space Research</title></titleInfo><titleInfo type="abbreviated"><title>JASR</title></titleInfo><genre type="journal">journal</genre><originInfo><dateIssued encoding="w3cdtf">199404</dateIssued></originInfo><identifier type="ISSN">0273-1177</identifier><identifier type="PII">S0273-1177(00)X0309-2</identifier><part><date>199404</date><detail type="volume"><number>14</number><caption>vol.</caption></detail><detail type="issue"><number>4</number><caption>no.</caption></detail><extent unit="issue pages"><start>1</start><end>203</end></extent><extent unit="pages"><start>181</start><end>194</end></extent></part></relatedItem><identifier type="istex">3776E4854B29AD2ED75E0CC816696BBECA7F0424</identifier><identifier type="DOI">10.1016/0273-1177(94)90181-3</identifier><identifier type="PII">0273-1177(94)90181-3</identifier><recordInfo><recordContentSource>ELSEVIER</recordContentSource></recordInfo></mods></metadata></istex></record>Pour manipuler ce document sous Unix (Dilib)
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