Composition of quasi‐stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer
Identifieur interne : 001366 ( Istex/Corpus ); précédent : 001365; suivant : 001367Composition of quasi‐stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer
Auteurs : R. Von Steiger ; N. A. Schwadron ; L. A. Fisk ; J. Geiss ; G. Gloeckler ; S. Hefti ; B. Wilken ; R. R. Wimmer Chweingruber ; T. H. ZurbuchenSource :
- Journal of Geophysical Research: Space Physics [ 0148-0227 ] ; 2000-12-01.
Abstract
Using improved, self‐consistent analysis techniques, we determine the average solar wind charge state and elemental composition of nearly 40 ion species of He, C, N, O, Ne, Mg, Si, S, and Fe observed with the Solar Wind Ion Composition Spectrometer on Ulysses. We compare results obtained during selected time periods, including both slow solar wind and fast streams, concentrating on the quasi‐stationary flows away from recurrent or intermittent disturbances such as corotating interaction regions or coronal mass ejections. In the fast streams the charge state distributions are consistent with a single freezing‐in temperature for each element, whereas in the slow wind these distributions appear to be composed of contributions from a range of temperatures. The elemental composition shows the well‐known first ionization potential (FIP) bias of the solar wind composition with respect to the photosphere. However, it appears that our average enrichment factor of low‐FIP elements in the slow wind, not quite a factor of 3, is smaller than that in previous compilations. In fast streams the FIP bias is found to be yet smaller but still significantly above 1, clearly indicating that the FIP fractionation effect is also active beneath coronal holes from where the fast wind originates. This imposes basic requirements upon FIP fractionation models, which should reproduce the stronger and more variable low‐FIP bias in the slow wind and a weaker (and perhaps conceptually different) low‐FIP bias in fast streams. Taken together, these results firmly establish the fundamental difference between the two quasi‐stationary solar wind types.
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DOI: 10.1029/1999JA000358
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Res.</title><idno type="ISSN">0148-0227</idno><idno type="eISSN">2156-2202</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><date type="published" when="2000-12-01">2000-12-01</date><biblScope unit="volume">105</biblScope><biblScope unit="issue">A12</biblScope><biblScope unit="page" from="27217">27217</biblScope><biblScope unit="page" to="27238">27238</biblScope></imprint><idno type="ISSN">0148-0227</idno></series><idno type="istex">C85B37DC10326CFC14C85F49911C6E3E18401C85</idno><idno type="DOI">10.1029/1999JA000358</idno><idno type="ArticleID">1999JA000358</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">Using improved, self‐consistent analysis techniques, we determine the average solar wind charge state and elemental composition of nearly 40 ion species of He, C, N, O, Ne, Mg, Si, S, and Fe observed with the Solar Wind Ion Composition Spectrometer on Ulysses. We compare results obtained during selected time periods, including both slow solar wind and fast streams, concentrating on the quasi‐stationary flows away from recurrent or intermittent disturbances such as corotating interaction regions or coronal mass ejections. In the fast streams the charge state distributions are consistent with a single freezing‐in temperature for each element, whereas in the slow wind these distributions appear to be composed of contributions from a range of temperatures. The elemental composition shows the well‐known first ionization potential (FIP) bias of the solar wind composition with respect to the photosphere. However, it appears that our average enrichment factor of low‐FIP elements in the slow wind, not quite a factor of 3, is smaller than that in previous compilations. In fast streams the FIP bias is found to be yet smaller but still significantly above 1, clearly indicating that the FIP fractionation effect is also active beneath coronal holes from where the fast wind originates. This imposes basic requirements upon FIP fractionation models, which should reproduce the stronger and more variable low‐FIP bias in the slow wind and a weaker (and perhaps conceptually different) low‐FIP bias in fast streams. Taken together, these results firmly establish the fundamental difference between the two quasi‐stationary solar wind types.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>R. von Steiger</name></json:item><json:item><name>N. A. Schwadron</name></json:item><json:item><name>L. A. Fisk</name></json:item><json:item><name>J. Geiss</name></json:item><json:item><name>G. Gloeckler</name></json:item><json:item><name>S. Hefti</name></json:item><json:item><name>B. Wilken</name></json:item><json:item><name>R. R. 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The elemental composition shows the well‐known first ionization potential (FIP) bias of the solar wind composition with respect to the photosphere. However, it appears that our average enrichment factor of low‐FIP elements in the slow wind, not quite a factor of 3, is smaller than that in previous compilations. In fast streams the FIP bias is found to be yet smaller but still significantly above 1, clearly indicating that the FIP fractionation effect is also active beneath coronal holes from where the fast wind originates. This imposes basic requirements upon FIP fractionation models, which should reproduce the stronger and more variable low‐FIP bias in the slow wind and a weaker (and perhaps conceptually different) low‐FIP bias in fast streams. 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We compare results obtained during selected time periods, including both slow solar wind and fast streams, concentrating on the quasi‐stationary flows away from recurrent or intermittent disturbances such as corotating interaction regions or coronal mass ejections. In the fast streams the charge state distributions are consistent with a single freezing‐in temperature for each element, whereas in the slow wind these distributions appear to be composed of contributions from a range of temperatures. The elemental composition shows the well‐known first ionization potential (FIP) bias of the solar wind composition with respect to the photosphere. However, it appears that our average enrichment factor of low‐FIP elements in the slow wind, not quite a factor of 3, is smaller than that in previous compilations. In fast streams the FIP bias is found to be yet smaller but still significantly above 1, clearly indicating that the FIP fractionation effect is also active beneath coronal holes from where the fast wind originates. This imposes basic requirements upon FIP fractionation models, which should reproduce the stronger and more variable low‐FIP bias in the slow wind and a weaker (and perhaps conceptually different) low‐FIP bias in fast streams. 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A.</givenNames> <familyName>Schwadron</familyName></author>, <author><givenNames>L. A.</givenNames> <familyName>Fisk</familyName></author>, <author><givenNames>J.</givenNames> <familyName>Geiss</familyName></author>, <author><givenNames>G.</givenNames> <familyName>Gloeckler</familyName></author>, <author><givenNames>S.</givenNames> <familyName>Hefti</familyName></author>, <author><givenNames>B.</givenNames> <familyName>Wilken</familyName></author>, <author><givenNames>R. R.</givenNames> <familyName>Wimmer‐Schweingruber</familyName></author>, and <author><givenNames>T. H.</givenNames> <familyName>Zurbuchen</familyName></author> (<pubYear year="2000">2000</pubYear>), <articleTitle>Composition of quasi‐stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer</articleTitle>, <journalTitle>J. Geophys. 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A.</givenNames><familyName>Fisk</familyName></personName></creator><creator xml:id="jgra14966-cr-0004"><personName><givenNames>J.</givenNames><familyName>Geiss</familyName></personName></creator><creator xml:id="jgra14966-cr-0005"><personName><givenNames>G.</givenNames><familyName>Gloeckler</familyName></personName></creator><creator xml:id="jgra14966-cr-0006"><personName><givenNames>S.</givenNames><familyName>Hefti</familyName></personName></creator><creator xml:id="jgra14966-cr-0007"><personName><givenNames>B.</givenNames><familyName>Wilken</familyName></personName></creator><creator xml:id="jgra14966-cr-0008"><personName><givenNames>R. R.</givenNames><familyName>Wimmer‐Schweingruber</familyName></personName></creator><creator xml:id="jgra14966-cr-0009"><personName><givenNames>T. H.</givenNames><familyName>Zurbuchen</familyName></personName></creator></creators><abstractGroup><abstract type="main"><p xml:id="jgra14966-para-0001">Using improved, self‐consistent analysis techniques, we determine the average solar wind charge state and elemental composition of nearly 40 ion species of He, C, N, O, Ne, Mg, Si, S, and Fe observed with the Solar Wind Ion Composition Spectrometer on Ulysses. We compare results obtained during selected time periods, including both slow solar wind and fast streams, concentrating on the quasi‐stationary flows away from recurrent or intermittent disturbances such as corotating interaction regions or coronal mass ejections. In the fast streams the charge state distributions are consistent with a single freezing‐in temperature for each element, whereas in the slow wind these distributions appear to be composed of contributions from a range of temperatures. The elemental composition shows the well‐known first ionization potential (FIP) bias of the solar wind composition with respect to the photosphere. However, it appears that our average enrichment factor of low‐FIP elements in the slow wind, not quite a factor of 3, is smaller than that in previous compilations. In fast streams the FIP bias is found to be yet smaller but still significantly above 1, clearly indicating that the FIP fractionation effect is also active beneath coronal holes from where the fast wind originates. This imposes basic requirements upon FIP fractionation models, which should reproduce the stronger and more variable low‐FIP bias in the slow wind and a weaker (and perhaps conceptually different) low‐FIP bias in fast streams. Taken together, these results firmly establish the fundamental difference between the two quasi‐stationary solar wind types.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Composition of quasi‐stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Composition of quasi‐stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer</title></titleInfo><name type="personal"><namePart type="given">R.</namePart><namePart type="family">von Steiger</namePart></name><name type="personal"><namePart type="given">N. A.</namePart><namePart type="family">Schwadron</namePart></name><name type="personal"><namePart type="given">L. A.</namePart><namePart type="family">Fisk</namePart></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Geiss</namePart></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Gloeckler</namePart></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Hefti</namePart></name><name type="personal"><namePart type="given">B.</namePart><namePart type="family">Wilken</namePart></name><name type="personal"><namePart type="given">R. R.</namePart><namePart type="family">Wimmer‐Schweingruber</namePart></name><name type="personal"><namePart type="given">T. H.</namePart><namePart type="family">Zurbuchen</namePart></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><dateIssued encoding="w3cdtf">2000-12-01</dateIssued><dateCaptured encoding="w3cdtf">1999-09-27</dateCaptured><dateValid encoding="w3cdtf">2000-07-05</dateValid><edition>vonSteiger, R., N. A. Schwadron, L. A. Fisk, J. Geiss, G. Gloeckler, S. Hefti, B. Wilken, R. R. Wimmer‐Schweingruber, and T. H. Zurbuchen (2000), Composition of quasi‐stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer, J. Geophys. Res., 105(A12), 27217–27238, doi:10.1029/1999JA000358.</edition><copyrightDate encoding="w3cdtf">2000</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>Using improved, self‐consistent analysis techniques, we determine the average solar wind charge state and elemental composition of nearly 40 ion species of He, C, N, O, Ne, Mg, Si, S, and Fe observed with the Solar Wind Ion Composition Spectrometer on Ulysses. We compare results obtained during selected time periods, including both slow solar wind and fast streams, concentrating on the quasi‐stationary flows away from recurrent or intermittent disturbances such as corotating interaction regions or coronal mass ejections. In the fast streams the charge state distributions are consistent with a single freezing‐in temperature for each element, whereas in the slow wind these distributions appear to be composed of contributions from a range of temperatures. The elemental composition shows the well‐known first ionization potential (FIP) bias of the solar wind composition with respect to the photosphere. However, it appears that our average enrichment factor of low‐FIP elements in the slow wind, not quite a factor of 3, is smaller than that in previous compilations. In fast streams the FIP bias is found to be yet smaller but still significantly above 1, clearly indicating that the FIP fractionation effect is also active beneath coronal holes from where the fast wind originates. This imposes basic requirements upon FIP fractionation models, which should reproduce the stronger and more variable low‐FIP bias in the slow wind and a weaker (and perhaps conceptually different) low‐FIP bias in fast streams. Taken together, these results firmly establish the fundamental difference between the two quasi‐stationary solar wind types.</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>index-terms</genre><topic authorityURI="http://psi.agu.org/taxonomy5/2100">INTERPLANETARY PHYSICS</topic><topic authorityURI="http://psi.agu.org/taxonomy5/2164">Solar wind plasma</topic><topic authorityURI="http://psi.agu.org/taxonomy5/2169">Solar wind sources</topic><topic authorityURI="http://psi.agu.org/taxonomy5/2194">Instruments and techniques</topic></subject><subject><genre>article-category</genre><topic>Papers on Solar and Heliospheric Physics</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>2000</date><detail type="volume"><caption>vol.</caption><number>105</number></detail><detail type="issue"><caption>no.</caption><number>A12</number></detail><extent unit="pages"><start>27217</start><end>27238</end><total>22</total></extent></part></relatedItem><identifier type="istex">C85B37DC10326CFC14C85F49911C6E3E18401C85</identifier><identifier type="DOI">10.1029/1999JA000358</identifier><identifier type="ArticleID">1999JA000358</identifier><accessCondition type="use and reproduction" contentType="copyright">Copyright 2000 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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