Observation of the impulsive phase of a simple flare
Identifieur interne : 000760 ( Main/Corpus ); précédent : 000759; suivant : 000761Observation of the impulsive phase of a simple flare
Auteurs : E. Tandberg-Hanssen ; P. Kaufmann ; J. Reichmann ; L. Teuber ; L. Moore ; E. Orwig ; H. ZirinSource :
- Solar Physics [ 0038-0938 ] ; 1984-01-01.
Abstract
Abstract: We present a broad range of complementary observations of the onset and impulsive phase of a fairly large (1B, M1.2) but simple two-ribbon flare. The observations consist of hard X-ray flux measured by the SMM HXRBS, high-sensitivity measurements of microwave flux at 22 GHz from Itapetinga Radio Observatory, sequences of spectroheliograms in UV emission lines from Ov (T ≈ 2 × 105 K) and Fexxi (T ≈ 1 × 107 K) from the SMM UVSP, Hα and Hei D3 cine-filtergrams from Big Bear Solar Observatory, and a magnetogram of the flare region from the MSFC Solar Observatory. From these data we conclude: (1) The overall magnetic field configuration in which the flare occurred was a fairly simple, closed arch containing nonpotential substructure. (2) The flare occurred spontaneously within the arch; it was not triggered by emerging magnetic flux. (3) The impulsive energy release occurred in two major spikes. The second spike took place within the flare arch heated in the first spike, but was concentrated on a different subset of field lines. The ratio of Ov emission to hard X-ray emission decreased by at least a factor of 2 from the first spike to the second, probably because the plasma density in the flare arch had increased by chromospheric evaporation. (4) The impulsive energy release most likely occurred in the upper part of the arch; it had three immediate products: (a) An increase in the plasma pressure throughout the flare arch of at least a factor of 10. This is required because the Fexxi emission was confined to the feet of the flare arch for at least the first minute of the impulsive phase. (b) Nonthermal energetic (∼ 25 keV) electrons which impacted the feet of the arch to produce the hard X-ray burst and impulsive brightening in Ov and D3. The evidence for this is the simultaneity, within ± 2 s, of the peak Ov and hard X-ray emissions. (c) Another population of high-energy (∼100keV) electrons (decoupled from the population that produced the hard X-rays) that produced the impulsive microwave emission at 22 GHz. This conclusion is drawn because the microwave peak was 6 ± 3 s later than the hard X-ray peak.
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DOI: 10.1007/BF00153784
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Tandberg-Hanssen</name><affiliation><mods:affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</mods:affiliation></affiliation></author><author><name sortKey="Kaufmann, P" sort="Kaufmann, P" uniqKey="Kaufmann P" first="P." last="Kaufmann">P. Kaufmann</name><affiliation><mods:affiliation>INPE, Institute de Pesquisas Espaciais, 12200, S. José dos Campos, SP Brazil</mods:affiliation></affiliation></author><author><name sortKey="Reichmann, J" sort="Reichmann, J" uniqKey="Reichmann J" first="J." last="Reichmann">J. Reichmann</name><affiliation><mods:affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</mods:affiliation></affiliation></author><author><name sortKey="Teuber, L" sort="Teuber, L" uniqKey="Teuber L" first="L." last="Teuber">L. Teuber</name><affiliation><mods:affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</mods:affiliation></affiliation></author><author><name sortKey="Moore, L" sort="Moore, L" uniqKey="Moore L" first="L." last="Moore">L. Moore</name><affiliation><mods:affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</mods:affiliation></affiliation></author><author><name sortKey="Orwig, E" sort="Orwig, E" uniqKey="Orwig E" first="E." last="Orwig">E. Orwig</name><affiliation><mods:affiliation>NASA, Goddard Space Flight Center, 20771, MD, U.S.A.</mods:affiliation></affiliation><affiliation><mods:affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</mods:affiliation></affiliation></author><author><name sortKey="Zirin, H" sort="Zirin, H" uniqKey="Zirin H" first="H." last="Zirin">H. Zirin</name><affiliation><mods:affiliation>Big Bear Solar Observatory, 91125, Caltech, Pasadena, CA, U.S.A.</mods:affiliation></affiliation><affiliation><mods:affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</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="1984-01-01">1984-01-01</date><biblScope unit="volume">90</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="41">41</biblScope><biblScope unit="page" to="62">62</biblScope></imprint><idno type="ISSN">0038-0938</idno></series><idno type="istex">BC0501FFCBC5AC081ADA105B643160B0A730002C</idno><idno type="DOI">10.1007/BF00153784</idno><idno type="ArticleID">BF00153784</idno><idno type="ArticleID">Art6</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: We present a broad range of complementary observations of the onset and impulsive phase of a fairly large (1B, M1.2) but simple two-ribbon flare. The observations consist of hard X-ray flux measured by the SMM HXRBS, high-sensitivity measurements of microwave flux at 22 GHz from Itapetinga Radio Observatory, sequences of spectroheliograms in UV emission lines from Ov (T ≈ 2 × 105 K) and Fexxi (T ≈ 1 × 107 K) from the SMM UVSP, Hα and Hei D3 cine-filtergrams from Big Bear Solar Observatory, and a magnetogram of the flare region from the MSFC Solar Observatory. From these data we conclude: (1) The overall magnetic field configuration in which the flare occurred was a fairly simple, closed arch containing nonpotential substructure. (2) The flare occurred spontaneously within the arch; it was not triggered by emerging magnetic flux. (3) The impulsive energy release occurred in two major spikes. The second spike took place within the flare arch heated in the first spike, but was concentrated on a different subset of field lines. The ratio of Ov emission to hard X-ray emission decreased by at least a factor of 2 from the first spike to the second, probably because the plasma density in the flare arch had increased by chromospheric evaporation. (4) The impulsive energy release most likely occurred in the upper part of the arch; it had three immediate products: (a) An increase in the plasma pressure throughout the flare arch of at least a factor of 10. This is required because the Fexxi emission was confined to the feet of the flare arch for at least the first minute of the impulsive phase. (b) Nonthermal energetic (∼ 25 keV) electrons which impacted the feet of the arch to produce the hard X-ray burst and impulsive brightening in Ov and D3. The evidence for this is the simultaneity, within ± 2 s, of the peak Ov and hard X-ray emissions. (c) Another population of high-energy (∼100keV) electrons (decoupled from the population that produced the hard X-rays) that produced the impulsive microwave emission at 22 GHz. This conclusion is drawn because the microwave peak was 6 ± 3 s later than the hard X-ray peak.</div></front></TEI><istex><corpusName>springer</corpusName><author><json:item><name>E. Tandberg-Hanssen</name><affiliations><json:string>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</json:string></affiliations></json:item><json:item><name>P. Kaufmann</name><affiliations><json:string>INPE, Institute de Pesquisas Espaciais, 12200, S. José dos Campos, SP Brazil</json:string></affiliations></json:item><json:item><name>E. J. Reichmann</name><affiliations><json:string>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</json:string></affiliations></json:item><json:item><name>D. L. Teuber</name><affiliations><json:string>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</json:string></affiliations></json:item><json:item><name>R. L. Moore</name><affiliations><json:string>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</json:string></affiliations></json:item><json:item><name>L. E. Orwig</name><affiliations><json:string>NASA, Goddard Space Flight Center, 20771, MD, U.S.A.</json:string><json:string>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</json:string></affiliations></json:item><json:item><name>H. Zirin</name><affiliations><json:string>Big Bear Solar Observatory, 91125, Caltech, Pasadena, CA, U.S.A.</json:string><json:string>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</json:string></affiliations></json:item></author><articleId><json:string>BF00153784</json:string><json:string>Art6</json:string></articleId><language><json:string>eng</json:string></language><originalGenre><json:string>OriginalPaper</json:string></originalGenre><abstract>Abstract: We present a broad range of complementary observations of the onset and impulsive phase of a fairly large (1B, M1.2) but simple two-ribbon flare. The observations consist of hard X-ray flux measured by the SMM HXRBS, high-sensitivity measurements of microwave flux at 22 GHz from Itapetinga Radio Observatory, sequences of spectroheliograms in UV emission lines from Ov (T ≈ 2 × 105 K) and Fexxi (T ≈ 1 × 107 K) from the SMM UVSP, Hα and Hei D3 cine-filtergrams from Big Bear Solar Observatory, and a magnetogram of the flare region from the MSFC Solar Observatory. From these data we conclude: (1) The overall magnetic field configuration in which the flare occurred was a fairly simple, closed arch containing nonpotential substructure. (2) The flare occurred spontaneously within the arch; it was not triggered by emerging magnetic flux. (3) The impulsive energy release occurred in two major spikes. The second spike took place within the flare arch heated in the first spike, but was concentrated on a different subset of field lines. The ratio of Ov emission to hard X-ray emission decreased by at least a factor of 2 from the first spike to the second, probably because the plasma density in the flare arch had increased by chromospheric evaporation. (4) The impulsive energy release most likely occurred in the upper part of the arch; it had three immediate products: (a) An increase in the plasma pressure throughout the flare arch of at least a factor of 10. This is required because the Fexxi emission was confined to the feet of the flare arch for at least the first minute of the impulsive phase. (b) Nonthermal energetic (∼ 25 keV) electrons which impacted the feet of the arch to produce the hard X-ray burst and impulsive brightening in Ov and D3. The evidence for this is the simultaneity, within ± 2 s, of the peak Ov and hard X-ray emissions. (c) Another population of high-energy (∼100keV) electrons (decoupled from the population that produced the hard X-rays) that produced the impulsive microwave emission at 22 GHz. 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Reidel Publishing Company, 1984</p></availability><date>1983-09-05</date></publicationStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">Observation of the impulsive phase of a simple flare</title><author xml:id="author-1"><persName><forename type="first">E.</forename><surname>Tandberg-Hanssen</surname></persName><affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</affiliation></author><author xml:id="author-2"><persName><forename type="first">P.</forename><surname>Kaufmann</surname></persName><affiliation>INPE, Institute de Pesquisas Espaciais, 12200, S. 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The observations consist of hard X-ray flux measured by the SMM HXRBS, high-sensitivity measurements of microwave flux at 22 GHz from Itapetinga Radio Observatory, sequences of spectroheliograms in UV emission lines from Ov (T ≈ 2 × 105 K) and Fexxi (T ≈ 1 × 107 K) from the SMM UVSP, Hα and Hei D3 cine-filtergrams from Big Bear Solar Observatory, and a magnetogram of the flare region from the MSFC Solar Observatory. From these data we conclude: (1) The overall magnetic field configuration in which the flare occurred was a fairly simple, closed arch containing nonpotential substructure. (2) The flare occurred spontaneously within the arch; it was not triggered by emerging magnetic flux. (3) The impulsive energy release occurred in two major spikes. The second spike took place within the flare arch heated in the first spike, but was concentrated on a different subset of field lines. The ratio of Ov emission to hard X-ray emission decreased by at least a factor of 2 from the first spike to the second, probably because the plasma density in the flare arch had increased by chromospheric evaporation. (4) The impulsive energy release most likely occurred in the upper part of the arch; it had three immediate products: (a) An increase in the plasma pressure throughout the flare arch of at least a factor of 10. This is required because the Fexxi emission was confined to the feet of the flare arch for at least the first minute of the impulsive phase. (b) Nonthermal energetic (∼ 25 keV) electrons which impacted the feet of the arch to produce the hard X-ray burst and impulsive brightening in Ov and D3. The evidence for this is the simultaneity, within ± 2 s, of the peak Ov and hard X-ray emissions. (c) Another population of high-energy (∼100keV) electrons (decoupled from the population that produced the hard X-rays) that produced the impulsive microwave emission at 22 GHz. This conclusion is drawn because the microwave peak was 6 ± 3 s later than the hard X-ray peak.</p></abstract><textClass><keywords scheme="Journal Subject"><list><head>Physics</head><item><term>Astrophysics</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="1983-09-05">Created</change><change when="1984-01-01">Published</change><change xml:id="refBibs-istex" who="#ISTEX-API" when="2016-09-22">References added</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/BC0501FFCBC5AC081ADA105B643160B0A730002C/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>90</VolumeIDStart><VolumeIDEnd>90</VolumeIDEnd><VolumeIssueCount>2</VolumeIssueCount></VolumeInfo><Issue IssueType="Regular"><IssueInfo TocLevels="0"><IssueIDStart>1</IssueIDStart><IssueIDEnd>1</IssueIDEnd><IssueArticleCount>20</IssueArticleCount><IssueHistory><CoverDate><Year>1984</Year><Month>1</Month></CoverDate></IssueHistory><IssueCopyright><CopyrightHolderName>D. Reidel Publishing Company</CopyrightHolderName><CopyrightYear>1984</CopyrightYear></IssueCopyright></IssueInfo><Article ID="Art6"><ArticleInfo Language="En" ArticleType="OriginalPaper" NumberingStyle="Unnumbered" TocLevels="0" ContainsESM="No"><ArticleID>BF00153784</ArticleID><ArticleDOI>10.1007/BF00153784</ArticleDOI><ArticleSequenceNumber>6</ArticleSequenceNumber><ArticleTitle Language="En">Observation of the impulsive phase of a simple flare</ArticleTitle><ArticleFirstPage>41</ArticleFirstPage><ArticleLastPage>62</ArticleLastPage><ArticleHistory><RegistrationDate><Year>2004</Year><Month>6</Month><Day>22</Day></RegistrationDate><Received><Year>1983</Year><Month>9</Month><Day>5</Day></Received></ArticleHistory><ArticleCopyright><CopyrightHolderName>D. Reidel Publishing Company</CopyrightHolderName><CopyrightYear>1984</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>90</VolumeIDStart><VolumeIDEnd>90</VolumeIDEnd><IssueIDStart>1</IssueIDStart><IssueIDEnd>1</IssueIDEnd></ArticleContext></ArticleInfo><ArticleHeader><AuthorGroup><Author AffiliationIDS="Aff1"><AuthorName DisplayOrder="Western"><GivenName>E.</GivenName><FamilyName>Tandberg-Hanssen</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff2"><AuthorName DisplayOrder="Western"><GivenName>P.</GivenName><FamilyName>Kaufmann</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff1"><AuthorName DisplayOrder="Western"><GivenName>E.</GivenName><GivenName>J.</GivenName><FamilyName>Reichmann</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff1"><AuthorName DisplayOrder="Western"><GivenName>D.</GivenName><GivenName>L.</GivenName><FamilyName>Teuber</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff1"><AuthorName DisplayOrder="Western"><GivenName>R.</GivenName><GivenName>L.</GivenName><FamilyName>Moore</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff3 Aff1"><AuthorName DisplayOrder="Western"><GivenName>L.</GivenName><GivenName>E.</GivenName><FamilyName>Orwig</FamilyName></AuthorName></Author><Author AffiliationIDS="Aff4 Aff1"><AuthorName DisplayOrder="Western"><GivenName>H.</GivenName><FamilyName>Zirin</FamilyName></AuthorName></Author><Affiliation ID="Aff2"><OrgName>INPE, Institute de Pesquisas Espaciais</OrgName><OrgAddress><Postcode>12200</Postcode><City>S. José dos Campos</City><Country>SP Brazil</Country></OrgAddress></Affiliation><Affiliation ID="Aff3"><OrgName>NASA, Goddard Space Flight Center</OrgName><OrgAddress><Postcode>20771</Postcode><State>MD</State><Country>U.S.A.</Country></OrgAddress></Affiliation><Affiliation ID="Aff4"><OrgName>Big Bear Solar Observatory</OrgName><OrgAddress><Postcode>91125</Postcode><City>Caltech, Pasadena</City><State>CA</State><Country>U.S.A.</Country></OrgAddress></Affiliation><Affiliation ID="Aff1"><OrgName>NASA, Marshall Space Flight Center</OrgName><OrgAddress><Postcode>35812</Postcode><State>AL</State><Country>U.S.A.</Country></OrgAddress></Affiliation></AuthorGroup><Abstract ID="Abs1" Language="En"><Heading>Abstract</Heading><Para>We present a broad range of complementary observations of the onset and impulsive phase of a fairly large (1B, M1.2) but simple two-ribbon flare. The observations consist of hard X-ray flux measured by the SMM HXRBS, high-sensitivity measurements of microwave flux at 22 GHz from Itapetinga Radio Observatory, sequences of spectroheliograms in UV emission lines from Ov (<Emphasis Type="Italic">T</Emphasis> ≈ 2 × 10<Superscript>5</Superscript> K) and Fe<Emphasis Type="SmallCaps">xxi</Emphasis> (<Emphasis Type="Italic">T</Emphasis> ≈ 1 × 10<Superscript>7</Superscript> K) from the SMM UVSP, Hα and He<Emphasis Type="SmallCaps">i</Emphasis> D<Subscript>3</Subscript> cine-filtergrams from Big Bear Solar Observatory, and a magnetogram of the flare region from the MSFC Solar Observatory. From these data we conclude:<OrderedList><ListItem><ItemNumber>(1)</ItemNumber><ItemContent><Para>The overall magnetic field configuration in which the flare occurred was a fairly simple, closed arch containing nonpotential substructure.</Para></ItemContent></ListItem><ListItem><ItemNumber>(2)</ItemNumber><ItemContent><Para>The flare occurred spontaneously within the arch; it was not triggered by emerging magnetic flux.</Para></ItemContent></ListItem><ListItem><ItemNumber>(3)</ItemNumber><ItemContent><Para>The impulsive energy release occurred in two major spikes. The second spike took place within the flare arch heated in the first spike, but was concentrated on a different subset of field lines. The ratio of Ov emission to hard X-ray emission decreased by at least a factor of 2 from the first spike to the second, probably because the plasma density in the flare arch had increased by chromospheric evaporation.</Para></ItemContent></ListItem><ListItem><ItemNumber>(4)</ItemNumber><ItemContent><Para>The impulsive energy release most likely occurred in the upper part of the arch; it had three <Emphasis Type="Italic">immediate</Emphasis> products:</Para></ItemContent></ListItem></OrderedList><OrderedList><ListItem><ItemNumber>(a)</ItemNumber><ItemContent><Para>An increase in the plasma pressure throughout the flare arch of at least a factor of 10. This is required because the Fe<Emphasis Type="SmallCaps">xxi</Emphasis> emission was confined to the feet of the flare arch for at least the first minute of the impulsive phase.</Para></ItemContent></ListItem><ListItem><ItemNumber>(b)</ItemNumber><ItemContent><Para>Nonthermal energetic (∼ 25 keV) electrons which impacted the feet of the arch to produce the hard X-ray burst and impulsive brightening in Ov and D<Subscript>3</Subscript>. The evidence for this is the simultaneity, within ± 2 s, of the peak Ov and hard X-ray emissions.</Para></ItemContent></ListItem><ListItem><ItemNumber>(c)</ItemNumber><ItemContent><Para>Another population of high-energy (∼100keV) electrons (decoupled from the population that produced the hard X-rays) that produced the impulsive microwave emission at 22 GHz. This conclusion is drawn because the microwave peak was 6 ± 3 s later than the hard X-ray peak.</Para></ItemContent></ListItem></OrderedList></Para></Abstract></ArticleHeader><NoBody></NoBody></Article></Issue></Volume></Journal></Publisher></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Observation of the impulsive phase of a simple flare</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Observation of the impulsive phase of a simple flare</title></titleInfo><name type="personal"><namePart type="given">E.</namePart><namePart type="family">Tandberg-Hanssen</namePart><affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Kaufmann</namePart><affiliation>INPE, Institute de Pesquisas Espaciais, 12200, S. José dos Campos, SP Brazil</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E.</namePart><namePart type="given">J.</namePart><namePart type="family">Reichmann</namePart><affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="given">L.</namePart><namePart type="family">Teuber</namePart><affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="given">L.</namePart><namePart type="family">Moore</namePart><affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.</namePart><namePart type="given">E.</namePart><namePart type="family">Orwig</namePart><affiliation>NASA, Goddard Space Flight Center, 20771, MD, U.S.A.</affiliation><affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H.</namePart><namePart type="family">Zirin</namePart><affiliation>Big Bear Solar Observatory, 91125, Caltech, Pasadena, CA, U.S.A.</affiliation><affiliation>NASA, Marshall Space Flight Center, 35812, AL, U.S.A.</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">1983-09-05</dateCreated><dateIssued encoding="w3cdtf">1984-01-01</dateIssued><copyrightDate encoding="w3cdtf">1984</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: We present a broad range of complementary observations of the onset and impulsive phase of a fairly large (1B, M1.2) but simple two-ribbon flare. The observations consist of hard X-ray flux measured by the SMM HXRBS, high-sensitivity measurements of microwave flux at 22 GHz from Itapetinga Radio Observatory, sequences of spectroheliograms in UV emission lines from Ov (T ≈ 2 × 105 K) and Fexxi (T ≈ 1 × 107 K) from the SMM UVSP, Hα and Hei D3 cine-filtergrams from Big Bear Solar Observatory, and a magnetogram of the flare region from the MSFC Solar Observatory. From these data we conclude: (1) The overall magnetic field configuration in which the flare occurred was a fairly simple, closed arch containing nonpotential substructure. (2) The flare occurred spontaneously within the arch; it was not triggered by emerging magnetic flux. (3) The impulsive energy release occurred in two major spikes. The second spike took place within the flare arch heated in the first spike, but was concentrated on a different subset of field lines. The ratio of Ov emission to hard X-ray emission decreased by at least a factor of 2 from the first spike to the second, probably because the plasma density in the flare arch had increased by chromospheric evaporation. (4) The impulsive energy release most likely occurred in the upper part of the arch; it had three immediate products: (a) An increase in the plasma pressure throughout the flare arch of at least a factor of 10. This is required because the Fexxi emission was confined to the feet of the flare arch for at least the first minute of the impulsive phase. (b) Nonthermal energetic (∼ 25 keV) electrons which impacted the feet of the arch to produce the hard X-ray burst and impulsive brightening in Ov and D3. The evidence for this is the simultaneity, within ± 2 s, of the peak Ov and hard X-ray emissions. (c) Another population of high-energy (∼100keV) electrons (decoupled from the population that produced the hard X-rays) that produced the impulsive microwave emission at 22 GHz. This conclusion is drawn because the microwave peak was 6 ± 3 s later than the hard X-ray peak.</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">1984-01-01</dateIssued><copyrightDate encoding="w3cdtf">1984</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">20</identifier><identifier type="VolumeIssueCount">2</identifier><part><date>1984</date><detail type="volume"><number>90</number><caption>vol.</caption></detail><detail type="issue"><number>1</number><caption>no.</caption></detail><extent unit="pages"><start>41</start><end>62</end></extent></part><recordInfo><recordOrigin>D. Reidel Publishing Company, 1984</recordOrigin></recordInfo></relatedItem><identifier type="istex">BC0501FFCBC5AC081ADA105B643160B0A730002C</identifier><identifier type="DOI">10.1007/BF00153784</identifier><identifier type="ArticleID">BF00153784</identifier><identifier type="ArticleID">Art6</identifier><accessCondition type="use and reproduction" contentType="copyright">D. Reidel Publishing Company, 1984</accessCondition><recordInfo><recordContentSource>SPRINGER</recordContentSource><recordOrigin>D. 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