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dc.contributor.author
van Driel Gesztelyi, Lidia
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dc.contributor.author
Attrill, G. D. R.
dc.contributor.author
Démoulin, Pascal
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dc.contributor.author
Mandrini, Cristina Hemilse
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dc.contributor.author
Harra, L. K.
dc.date.available
2017-07-17T17:56:50Z
dc.date.issued
2008-12
dc.identifier.citation
van Driel Gesztelyi, Lidia; Attrill, G. D. R.; Démoulin, Pascal; Mandrini, Cristina Hemilse; Harra, L. K.; Why are CMEs large-scale coronal events: nature or nurture?; Copernicus Publications; Annales Geophysicae; 26; 12-2008; 3077-3088
dc.identifier.issn
0992-7689
dc.identifier.uri
http://hdl.handle.net/11336/20703
dc.description.abstract
The apparent contradiction between small-scale source regions of, and large-scale coronal response to, coronal mass ejections (CMEs) has been a long-standing puzzle. For some, CMEs are considered to be inherently large-scale events – eruptions in which a number of flux systems participate in an unspecified manner, while others consider magnetic reconnection in special global topologies to be responsible for the large-scale response of the lower corona to CME events. Some of these ideas may indeed be correct in specific cases. However, what is the key element which makes CMEs large-scale? Observations show that the extent of the coronal disturbance matches the angular width of the CME – an important clue, which does not feature strongly in any of the above suggestions. We review observational evidence for the large-scale nature of CME source regions and find them lacking. Then we compare different ideas regarding how CMEs evolve to become large-scale. The large-scale magnetic topology plays an important role in this process. There is amounting evidence, however, that the key process is magnetic reconnection between the CME and other magnetic structures. We outline a CME evolution model, which is able to account for all the key observational signatures of large-scale CMEs and presents a clear picture how large portions of the Sun become constituents of the CME. In this model reconnection is driven by the expansion of the CME core resulting from an over-pressure relative to the pressure in the CME's surroundings. This implies that the extent of the lower coronal signatures match the final angular width of the CME.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Copernicus Publications
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Sun: Corona
dc.subject
Sun: Coronal Mass Ejections
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Why are CMEs large-scale coronal events: nature or nurture?
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-07-17T13:33:11Z
dc.identifier.eissn
1432-0576
dc.journal.volume
26
dc.journal.pagination
3077-3088
dc.journal.pais
Alemania
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dc.journal.ciudad
Berlin
dc.description.fil
Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.description.fil
Fil: Attrill, G. D. R.. University College London; Estados Unidos
dc.description.fil
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
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: Harra, L. K.. University College London; Estados Unidos
dc.journal.title
Annales Geophysicae
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.5194/angeo-26-3077-2008
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://www.ann-geophys.net/26/3077/2008/
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