A Cosmic-ray Composition Controlled by Volatility and a/q Ratio. snr Shock Acceleration of gas and Dust
Identifieur interne : 000016 ( Istex/Corpus ); précédent : 000015; suivant : 000017A Cosmic-ray Composition Controlled by Volatility and a/q Ratio. snr Shock Acceleration of gas and Dust
Auteurs : Jean-Paul Meyer ; Luke O'C. Drury ; Donald C. EllisonSource :
- Space Science Reviews [ 0038-6308 ] ; 1998.
English descriptors
- Teeft :
- Abundance, Abundance relative, Acceleration efficiency, Apparent correlation, Astron, Astrophys, Binns, Cambridge university press, Cass, Chemical compound, Clue element, Companion paper, Condensation temperature, Conf, Coronal, Coronal composition, Coronal material, Cosmic abundance, Cosmic ray, Datum, Different volatility, Dominant solid compound, Dust grain, Element condensation temperature, Element overabundance, Element relative, Element volatility, Ellison, Energetic particle, Enhancement, Entire grain, Error bar, Excess relative, Ferrando, First ionization potential, Gcrs, Gcrs abundance, Gcrs composition, Gcrs overabundance, Gcrs ratio, General correlation, General pattern, General trend, Grain destruction product, Grain material, Grain silicate, Grevesse, Heavier specie, Heavy element, Higher temperature, Intermediate class, Interstellar circumstellar, Interstellar propagation, Large error, Large spread, Lighter one, Mass dependence, Mass effect, Mass fractionation, Meyer, Monotonic function, More refractory element, More volatile one, Much less, Noble gas, Nucleosynthesis, Nucleosynthesis calculation, Other element, Other hand, Other type, Overabundance, Possible source, Preferential acceleration, Proc, Reames, Refractory, Refractory element, Refractory element relative, Relevant parameter, Same gcrs, Secondary element, Separate site, Shock speed, Shock wave, Show intermediate overabundance, Significant fraction, Single site, Single step, Singular behavior, Slow chemical reprocessing, Solar abundance ratio, Solar composition, Solar corona, Solar energetic particle, Solar value, Solar wind, Solid dot, Solid square, Source abundance, Source abundance relative, Source ratio, Spallation error, Stellar, Systematic error, Time solar, Up limit, Various element, Various type, Vernois, Volatile, Volatile element, Volatile one, Volatility, Waddington, Weak enhancement, Webber, Wind material, World scientific.
Abstract
Abstract: The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).
Url:
DOI: 10.1023/A:1005081721214
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We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. 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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>11214</JournalID><JournalPrintISSN>0038-6308</JournalPrintISSN><JournalElectronicISSN>1572-9672</JournalElectronicISSN><JournalTitle>Space Science Reviews</JournalTitle><JournalAbbreviatedTitle>Space Science Reviews</JournalAbbreviatedTitle><JournalSubjectGroup><JournalSubject Type="Primary">Physics</JournalSubject><JournalSubject Type="Secondary">Astronomy, Astrophysics and Cosmology</JournalSubject><JournalSubject Type="Secondary">Extraterrestrial Physics, Space Sciences</JournalSubject></JournalSubjectGroup></JournalInfo><Volume><VolumeInfo TocLevels="0" VolumeType="Regular"><VolumeIDStart>86</VolumeIDStart><VolumeIDEnd>86</VolumeIDEnd><VolumeIssueCount>4</VolumeIssueCount></VolumeInfo><Issue IssueType="Combined"><IssueInfo TocLevels="0"><IssueIDStart>1</IssueIDStart><IssueIDEnd>4</IssueIDEnd><IssueArticleCount>24</IssueArticleCount><IssueHistory><CoverDate><DateString>07-1998</DateString><Year>1998</Year><Month>7</Month></CoverDate></IssueHistory><IssueCopyright><CopyrightHolderName>Kluwer Academic Publishers</CopyrightHolderName><CopyrightYear>1998</CopyrightYear></IssueCopyright></IssueInfo><Article ID="Art10"><ArticleInfo ArticleType="OriginalPaper" ContainsESM="No" Language="En" NumberingStyle="Unnumbered" TocLevels="0"><ArticleID>164786</ArticleID><ArticleDOI>10.1023/A:1005081721214</ArticleDOI><ArticleSequenceNumber>10</ArticleSequenceNumber><ArticleTitle Language="En">A Cosmic-ray Composition Controlled by Volatility and a/q Ratio. snr Shock Acceleration of gas and Dust</ArticleTitle><ArticleFirstPage>179</ArticleFirstPage><ArticleLastPage>201</ArticleLastPage><ArticleHistory><RegistrationDate><Year>2004</Year><Month>10</Month><Day>7</Day></RegistrationDate></ArticleHistory><ArticleCopyright><CopyrightHolderName>Kluwer Academic Publishers</CopyrightHolderName><CopyrightYear>1998</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>11214</JournalID><VolumeIDStart>86</VolumeIDStart><VolumeIDEnd>86</VolumeIDEnd><IssueIDStart>1</IssueIDStart><IssueIDEnd>4</IssueIDEnd></ArticleContext></ArticleInfo><ArticleHeader><AuthorGroup><Author AffiliationIDS="Aff1"><AuthorName DisplayOrder="Western"><GivenName>Jean-Paul</GivenName><FamilyName>Meyer</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff2"><AuthorName DisplayOrder="Western"><GivenName>Luke</GivenName><GivenName>O'C.</GivenName><FamilyName>Drury</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff3"><AuthorName DisplayOrder="Western"><GivenName>Donald</GivenName><GivenName>C.</GivenName><FamilyName>Ellison</FamilyName></AuthorName></Author><Affiliation ID="Aff1"><OrgDivision>Service d'Astrophysique</OrgDivision><OrgName>DSM/DAPNIA, CEA/Saclay</OrgName><OrgAddress><Postcode>91191</Postcode><City>Gif-sur- Yvette</City><Country>France</Country></OrgAddress></Affiliation><Affiliation ID="Aff2"><OrgDivision>School of Cosmic Physics</OrgDivision><OrgName>Dublin Institute for Advanced Studies</OrgName><OrgAddress><Street>5 Merrion Square</Street><City>Dublin 2</City><Country>Ireland</Country></OrgAddress></Affiliation><Affiliation ID="Aff3"><OrgDivision>Department of Physics</OrgDivision><OrgName>North Carolina State University</OrgName><OrgAddress><Postbox>Box 8202</Postbox><City>Raleigh</City><State>NC</State><Postcode>27695</Postcode><Country>U.S.A.</Country></OrgAddress></Affiliation></AuthorGroup><Abstract ID="Abs1" Language="En"><Heading>Abstract</Heading><Para>The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).</Para></Abstract><ArticleNote Type="Corrigendum"><SimplePara>This revised version was published online in June 2006 with corrections to the Cover Date.</SimplePara></ArticleNote></ArticleHeader><NoBody></NoBody></Article></Issue></Volume></Journal></Publisher></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>A Cosmic-ray Composition Controlled by Volatility and a/q Ratio. snr Shock Acceleration of gas and Dust</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>A Cosmic-ray Composition Controlled by Volatility and a/q Ratio. snr Shock Acceleration of gas and Dust</title></titleInfo><name type="personal"><namePart type="given">Jean-Paul</namePart><namePart type="family">Meyer</namePart><affiliation>Service d'Astrophysique, DSM/DAPNIA, CEA/Saclay, 91191, Gif-sur- Yvette, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Luke</namePart><namePart type="given">O'C.</namePart><namePart type="family">Drury</namePart><affiliation>School of Cosmic Physics, Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Donald</namePart><namePart type="given">C.</namePart><namePart type="family">Ellison</namePart><affiliation>Department of Physics, North Carolina State University, Box 8202, 27695, Raleigh, NC, U.S.A.</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="OriginalPaper" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Kluwer Academic Publishers</publisher><place><placeTerm type="text">Dordrecht</placeTerm></place><dateIssued encoding="w3cdtf">1998-07-01</dateIssued><copyrightDate encoding="w3cdtf">1998</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><abstract lang="en">Abstract: The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).</abstract><relatedItem type="host"><titleInfo><title>Space Science Reviews</title></titleInfo><titleInfo type="abbreviated"><title>Space Science Reviews</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><originInfo><publisher>Springer</publisher><dateIssued encoding="w3cdtf">1998-07-01</dateIssued><copyrightDate encoding="w3cdtf">1998</copyrightDate></originInfo><subject><genre>Physics</genre><topic>Astronomy, Astrophysics and Cosmology</topic><topic>Extraterrestrial Physics, Space Sciences</topic></subject><identifier type="ISSN">0038-6308</identifier><identifier type="eISSN">1572-9672</identifier><identifier type="JournalID">11214</identifier><identifier type="IssueArticleCount">24</identifier><identifier type="VolumeIssueCount">4</identifier><part><date>1998</date><detail type="volume"><number>86</number><caption>vol.</caption></detail><detail type="issue"><number>1-4</number><caption>no.</caption></detail><extent unit="pages"><start>179</start><end>201</end></extent></part><recordInfo><recordOrigin>Kluwer Academic Publishers, 1998</recordOrigin></recordInfo></relatedItem><identifier type="istex">760B46A79C0805716CE813895836C66A85B198DC</identifier><identifier type="ark">ark:/67375/VQC-N5NFN4MH-7</identifier><identifier type="DOI">10.1023/A:1005081721214</identifier><identifier type="ArticleID">164786</identifier><identifier type="ArticleID">Art10</identifier><accessCondition type="use and reproduction" contentType="copyright">Kluwer Academic Publishers, 1998</accessCondition><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-3XSW68JL-F">springer</recordContentSource><recordOrigin>Converted from (version 1.2.14) to MODS version 3.6.</recordOrigin><recordCreationDate encoding="w3cdtf">2020-05-29</recordCreationDate></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/ark:/67375/VQC-N5NFN4MH-7/record.json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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