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dc.contributor.author
Démoulin, Pascal
dc.contributor.author
Klein, K. L.
dc.contributor.author
Goff, C. P.
dc.contributor.author
van Driel Gesztelyi, Lidia
dc.contributor.author
Culhane, J. L.
dc.contributor.author
Mandrini, Cristina Hemilse
dc.contributor.author
Matthews, S. A.
dc.contributor.author
Harra, L. K.
dc.date.available
2017-07-18T19:01:22Z
dc.date.issued
2007-12
dc.identifier.citation
Démoulin, Pascal; Klein, K. L.; Goff, C. P.; van Driel Gesztelyi, Lidia; Culhane, J. L.; et al.; Decametric N burst: A consequence of the interaction of two coronal mass ejections; Springer; Solar Physics; 240; 2; 12-2007; 301-313
dc.identifier.issn
0038-0938
dc.identifier.uri
http://hdl.handle.net/11336/20842
dc.description.abstract
Radio emissions of electron beams in the solar corona and interplanetary space are tracers of the underlying magnetic configuration and of its evolution. We analyse radio observations from the Culgoora and WIND/WAVES spectrographs, in combination with SOHO/LASCO and SOHO/MDI data, to understand the origin of a type N burst originating from NOAA AR 10540 on January 20, 2004, and its relationship with type II and type III emissions. All bursts are related to the flares and the CME analysed in a previous paper (Goff et al., 2007). A very unusual feature of this event was a decametric type N burst, where a type III-like burst, drifting towards low frequencies (negative drift), changes drift first to positive, then again to negative. At metre wavelengths, i.e., heliocentric distances ≲1.5R⊙, these bursts are ascribed to electron beams bouncing in a closed loop. Neither U nor N bursts are expected at decametric wavelengths because closed quasi-static loops are not thought to extend to distances ≫1.5R⊙. We take the opportunity of the good multi-instrument coverage of this event to analyse the origin of type N bursts in the high corona. Reconnection of the expanding ejecta with the magnetic structure of a previous CME, launched about 8 hours earlier, injects electrons in the same manner as with type III bursts but into open field lines having a local dip and apex. The latter shape was created by magnetic reconnection between the expanding CME and neighbouring (open) streamer field lines. This particular flux tube shape in the high corona, between 5R⊙ and 10R⊙, explains the observed type N burst. Since the required magnetic configuration is only a transient phenomenon formed by reconnection, severe timing and topological constraints are present to form the observed decametric N burst. They are therefore expected to be rare features.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Springer
dc.rights
info:eu-repo/semantics/restrictedAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject.classification
Astronomía
dc.subject.classification
Ciencias Físicas
dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
dc.title
Decametric N burst: A consequence of the interaction of two coronal mass ejections
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-07-18T14:52:04Z
dc.journal.volume
240
dc.journal.number
2
dc.journal.pagination
301-313
dc.journal.pais
Alemania
dc.journal.ciudad
Berlin
dc.description.fil
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.description.fil
Fil: Klein, K. L.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.description.fil
Fil: Goff, C. P.. Mullard Space Science Laboratory; Reino Unido
dc.description.fil
Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.description.fil
Fil: Culhane, J. L.. Mullard Space Science Laboratory; Reino Unido
dc.description.fil
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
dc.description.fil
Fil: Matthews, S. A.. Mullard Space Science Laboratory; Reino Unido
dc.description.fil
Fil: Harra, L. K.. Mullard Space Science Laboratory; Reino Unido
dc.journal.title
Solar Physics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1007/s11207-006-0259-2
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007%2Fs11207-006-0259-2


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