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Where Do Solar Filaments Form?

Published online by Cambridge University Press:  06 January 2014

Duncan H Mackay ,
Victor Gaizauskas  and
Anthony R. Yeates
Duncan H Mackay
Affiliation:
School of Mathematics and Statistics, University of St Andrews, St Andrews, KY16 9SS, UK email: duncan@mcs.st-and.ac.uk
Victor Gaizauskas
Affiliation:
HIA, CNRC, 100 Sussex Drive, Ottawa, Ontario, Canada
Anthony R. Yeates
Affiliation:
Department of Mathematical Sciences, Durham University, Durham, UK
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Abstract

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In 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.

Keywords

Sun: filamentsSun: magnetic fieldsSun: prominences

References

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