Where do solar filaments form?

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DOIResolve DOI: http://doi.org/10.1017/S1743921313011484
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TypeArticle
Proceedings titleNature of Prominences and their Role in Space Weather: Proceedings of the 300th Symposium of the International Astronomical Union
Series titleProceedings of the International Astronomical Union; Volume 8
Conference300th symposium of the International Astronomical Union, June 10-16, 2013, Paris, France
ISSN1743-9213
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
LanguageEnglish
AffiliationNational Research Council Canada (NRC-CNRC); National Science Infrastructure
Peer reviewedYes
NPARC number21270880
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Record identifier3ed675f1-c651-4697-99c4-6878dfed69ad
Record created2014-02-17
Record modified2016-05-09
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