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Where Do Solar Filaments Form?

  • Duncan H Mackay (a1), Victor Gaizauskas (a2) and Anthony R. Yeates (a3)
Abstract
Abstract

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.

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This list contains references from the content that can be linked to their source. For a full set of references and notes please see the PDF or HTML where available.

K. Galsgaard & A. W. Longbottom 1999, ApJ, 510, 444

D. H. Mackay , V. Gaizauskas , & A. R. Yeates 2008, Solar Phys., 248, 51

F. Tang 1987, Solar Phys., 107, 233

E. Tandberg-Hanssen 1995, Astrophysics and Space Science Library, 199

A. A. van Ballegooijen & P. C. H. Martens 1989, ApJ, 343, 971

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Proceedings of the International Astronomical Union
  • ISSN: 1743-9213
  • EISSN: 1743-9221
  • URL: /core/journals/proceedings-of-the-international-astronomical-union
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