Flaring arches
Identifieur interne : 000912 ( Main/Exploration ); précédent : 000911; suivant : 000913Flaring arches
Auteurs : F. Martin [États-Unis] ; F. Švestka [Pays-Bas]Source :
- Solar Physics [ 0038-0938 ] ; 1988-03-01.
Abstract
Abstract: ‘Flaring arches” is a name assigned to a particular component of some flares. This component consists of X-ray and Hα emission which traverses a coronal arch from one to the other of its chromospheric footpoints. The primary footpoint is at the site of a flare. The secondary footpoint, tens of thousands of kilometers distant from the source flare, but in the same active region, brightens in Hα concurrent with the beginning of the hard X-ray burst at the primary site. From the inferred travel time of the initial exciting agent we deduce that high speed electron streams travelling through the arch must be the source of the initial excitation at the secondary footpoint. Subsequently, a more slowly moving agent gradually enhances the arch first in X-rays and subsequently in Hα, starting at the primary footpoint and propagating along the arch trajectory. The plasma flow in Hα shows clearly that material is injected into the arch from the site of the primary footpoint and later on, at least in some events, a part of it is also falling back. Thus a typical flaring arch has three, and perhaps four consecutive phases: (1) An early phase characterized by the onset of hard X-ray burst and brightening of the secondary footpoint in Hα. (2) The main X-ray phase, during which X-ray emission propagates through the arch. (3) The main Hα phase, during which Hα emitting material propagates through the arch. And (4) an aftermath phase when some parts of the ejected material seem to flow in the reverse direction towards the primary site of injection. An extensive series of flaring arches was observed from 6 to 13 November, 1980 at the Big Bear Solar Observatory and with the Hard X-Ray Imaging Spectrometer (HXIS) on board the SMM in a magnetically complex active region. The two most intense arches for which complete Hα and X-ray data are available and which occurred on 6 November at 17 ∶ 21 UT (length ≈ 57000 km) and on 12 November at 16 ∶ 57 UT (length ≈ 263 000 km) are discussed in this paper.
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DOI: 10.1007/BF00171717
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Švestka</name></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:F9862A5CA1643F086FC3F226FCFEF82640A7BE2D</idno><date when="1988" year="1988">1988</date><idno type="doi">10.1007/BF00171717</idno><idno type="url">https://api.istex.fr/document/F9862A5CA1643F086FC3F226FCFEF82640A7BE2D/fulltext/pdf</idno><idno type="wicri:Area/Main/Corpus">000231</idno><idno type="wicri:Area/Main/Curation">000231</idno><idno type="wicri:Area/Main/Exploration">000912</idno><idno type="wicri:explorRef" wicri:stream="Main" wicri:step="Exploration">000912</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main" xml:lang="en">Flaring arches</title><author><name sortKey="Martin, F" sort="Martin, F" uniqKey="Martin F" first="F." last="Martin">F. Martin</name><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Solar Astronomy, CALTECH, 91125, Pasadena, CA</wicri:regionArea><wicri:noRegion>CA</wicri:noRegion></affiliation></author><author><name sortKey="Svestka, F" sort="Svestka, F" uniqKey="Svestka F" first="F." last="Švestka">F. Švestka</name><affiliation wicri:level="1"><country xml:lang="fr">Pays-Bas</country><wicri:regionArea>Laboratory for Space Research, SRON</wicri:regionArea><wicri:noRegion>SRON</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="1988-03-01">1988-03-01</date><biblScope unit="volume">116</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="91">91</biblScope><biblScope unit="page" to="118">118</biblScope></imprint><idno type="ISSN">0038-0938</idno></series><idno type="istex">F9862A5CA1643F086FC3F226FCFEF82640A7BE2D</idno><idno type="DOI">10.1007/BF00171717</idno><idno type="ArticleID">BF00171717</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: ‘Flaring arches” is a name assigned to a particular component of some flares. This component consists of X-ray and Hα emission which traverses a coronal arch from one to the other of its chromospheric footpoints. The primary footpoint is at the site of a flare. The secondary footpoint, tens of thousands of kilometers distant from the source flare, but in the same active region, brightens in Hα concurrent with the beginning of the hard X-ray burst at the primary site. From the inferred travel time of the initial exciting agent we deduce that high speed electron streams travelling through the arch must be the source of the initial excitation at the secondary footpoint. Subsequently, a more slowly moving agent gradually enhances the arch first in X-rays and subsequently in Hα, starting at the primary footpoint and propagating along the arch trajectory. The plasma flow in Hα shows clearly that material is injected into the arch from the site of the primary footpoint and later on, at least in some events, a part of it is also falling back. Thus a typical flaring arch has three, and perhaps four consecutive phases: (1) An early phase characterized by the onset of hard X-ray burst and brightening of the secondary footpoint in Hα. (2) The main X-ray phase, during which X-ray emission propagates through the arch. (3) The main Hα phase, during which Hα emitting material propagates through the arch. And (4) an aftermath phase when some parts of the ejected material seem to flow in the reverse direction towards the primary site of injection. An extensive series of flaring arches was observed from 6 to 13 November, 1980 at the Big Bear Solar Observatory and with the Hard X-Ray Imaging Spectrometer (HXIS) on board the SMM in a magnetically complex active region. The two most intense arches for which complete Hα and X-ray data are available and which occurred on 6 November at 17 ∶ 21 UT (length ≈ 57000 km) and on 12 November at 16 ∶ 57 UT (length ≈ 263 000 km) are discussed in this paper.</div></front></TEI><affiliations><list><country><li>Pays-Bas</li><li>États-Unis</li></country></list><tree><country name="États-Unis"><noRegion><name sortKey="Martin, F" sort="Martin, F" uniqKey="Martin F" first="F." last="Martin">F. Martin</name></noRegion></country><country name="Pays-Bas"><noRegion><name sortKey="Svestka, F" sort="Svestka, F" uniqKey="Svestka F" first="F." last="Švestka">F. Švestka</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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