Where do solar filaments form?

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DOIResolve DOI: http://doi.org/10.1017/S1743921313011484
AuthorSearch for: ; Search for: ; Search for:
TypeArticle
Proceedings titleNature of Prominences and their Role in Space Weather
Series titleProceedings of the International Astronomical Union; Volume 8
Conference300th symposium of the International Astronomical Union, June 10-16, 2013, Paris, France
ISSN1743-9213
1743-9221
ISBN9781107045194
Pages445446; # of pages: 2
AbstractIn the present study, we consider where large, stable solar filaments form relative to underlying magnetic polarities. We find that 92% of all large stable filaments form in magnetic configurations involving the interaction of two or more bipoles. Only 7% form above the Polarity Inversion Line (PIL) of a single bipole. This indicates that a key element in the formation of largescale stable filaments is the convergence of magnetic flux, resulting in either flux cancellation or coronal reconnection.
Publication date
PublisherCambridge University Press
International Astronomical Union
LanguageEnglish
AffiliationNational Research Council Canada (NRC-CNRC); NRC Herzberg Institute of Astrophysics
Peer reviewedYes
NPARC number21270880
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Record identifier3ed675f1-c651-4697-99c4-6878dfed69ad
Record created2014-02-17
Record modified2017-06-27
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