Where Do Solar Filaments Form?
2013 ◽
Vol 8
(S300)
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pp. 445-446
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Keyword(s):
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 large-scale stable filaments is the convergence of magnetic flux, resulting in either flux cancellation or coronal reconnection.
2000 ◽
Vol 179
◽
pp. 205-208
Keyword(s):
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2013 ◽
Vol 8
(S300)
◽
pp. 412-413
Keyword(s):
2013 ◽
Vol 8
(S300)
◽
pp. 121-124
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2010 ◽
Vol 6
(S273)
◽
pp. 15-20
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2011 ◽
Vol 116
(A2)
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pp. n/a-n/a
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