Study of the post-flare loops on 29 July 1973
Identifieur interne : 000965 ( Main/Exploration ); précédent : 000964; suivant : 000966Study of the post-flare loops on 29 July 1973
Auteurs : Z. Švestka [Pays-Bas, États-Unis] ; W. Dodson-Prince [États-Unis] ; F. Martin [États-Unis] ; C. Mohler [États-Unis] ; L. Moore [États-Unis] ; T. Nolte [États-Unis] ; D. Petrasso [États-Unis]Source :
- Solar Physics [ 0038-0938 ] ; 1982-06-01.
Abstract
Abstract: We present revised values of temperature and density for the flare loops of 29 July 1973 and compare the revised parameters with those obtained aboard the SMM for the two-ribbon flare of 21 May 1980. The 21 May flare occurred in a developed sunspot group; the 29 July event was a spotless two-ribbon flare. We find that the loops in the spotless flare extended higher (by a factor of 1.4–2.2), were less dense (by a factor of 5 or more in the first hour of development), were generally hotter, and the whole loop system decayed much slower than in the spotted flare (i.e. staying at higher temperature for a longer time). We also align the hot X-ray loops of the 29 July flare with the bright Hα ribbons and show that the Hα emission is brightest at the places where the spatial density of the hot elementary loops is enhanced.
Url:
DOI: 10.1007/BF00151609
Affiliations:
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Švestka</name><affiliation wicri:level="3"><country xml:lang="fr">Pays-Bas</country><wicri:regionArea>Space Research Laboratory, Utrecht</wicri:regionArea><placeName><settlement type="city">Utrecht</settlement><region nuts="2" type="province">Utrecht (province)</region></placeName></affiliation><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Center for Astrophysics and Space Science, University of California, San Diego, La Jolla</wicri:regionArea><wicri:noRegion>La Jolla</wicri:noRegion></affiliation></author><author><name sortKey="Dodson Prince, W" sort="Dodson Prince, W" uniqKey="Dodson Prince W" first="W." last="Dodson-Prince">W. 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Nolte</name><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>American Science and Engineering, Inc., Cambridge, Mass.</wicri:regionArea><wicri:noRegion>Mass.</wicri:noRegion></affiliation></author><author><name sortKey="Petrasso, D" sort="Petrasso, D" uniqKey="Petrasso D" first="D." last="Petrasso">D. Petrasso</name><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>American Science and Engineering, Inc., Cambridge, Mass.</wicri:regionArea><wicri:noRegion>Mass.</wicri:noRegion></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="1982-06-01">1982-06-01</date><biblScope unit="volume">78</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="271">271</biblScope><biblScope unit="page" to="285">285</biblScope></imprint><idno type="ISSN">0038-0938</idno></series><idno type="istex">44F031F5761D79F6E7F9863630E71BF7D88A8C21</idno><idno type="DOI">10.1007/BF00151609</idno><idno type="ArticleID">BF00151609</idno><idno type="ArticleID">Art7</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 revised values of temperature and density for the flare loops of 29 July 1973 and compare the revised parameters with those obtained aboard the SMM for the two-ribbon flare of 21 May 1980. The 21 May flare occurred in a developed sunspot group; the 29 July event was a spotless two-ribbon flare. We find that the loops in the spotless flare extended higher (by a factor of 1.4–2.2), were less dense (by a factor of 5 or more in the first hour of development), were generally hotter, and the whole loop system decayed much slower than in the spotted flare (i.e. staying at higher temperature for a longer time). We also align the hot X-ray loops of the 29 July flare with the bright Hα ribbons and show that the Hα emission is brightest at the places where the spatial density of the hot elementary loops is enhanced.</div></front></TEI><affiliations><list><country><li>Pays-Bas</li><li>États-Unis</li></country><region><li>Californie</li><li>Michigan</li><li>Utrecht (province)</li></region><settlement><li>Utrecht</li></settlement></list><tree><country name="Pays-Bas"><region name="Utrecht (province)"><name sortKey="Svestka, Z" sort="Svestka, Z" uniqKey="Svestka Z" first="Z." last="Švestka">Z. Švestka</name></region></country><country name="États-Unis"><noRegion><name sortKey="Svestka, Z" sort="Svestka, Z" uniqKey="Svestka Z" first="Z." last="Švestka">Z. Švestka</name></noRegion><name sortKey="Dodson Prince, W" sort="Dodson Prince, W" uniqKey="Dodson Prince W" first="W." last="Dodson-Prince">W. Dodson-Prince</name><name sortKey="Martin, F" sort="Martin, F" uniqKey="Martin F" first="F." last="Martin">F. Martin</name><name sortKey="Mohler, C" sort="Mohler, C" uniqKey="Mohler C" first="C." last="Mohler">C. Mohler</name><name sortKey="Moore, L" sort="Moore, L" uniqKey="Moore L" first="L." last="Moore">L. Moore</name><name sortKey="Nolte, T" sort="Nolte, T" uniqKey="Nolte T" first="T." last="Nolte">T. Nolte</name><name sortKey="Petrasso, D" sort="Petrasso, D" uniqKey="Petrasso D" first="D." last="Petrasso">D. Petrasso</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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