Abstract
Filament channels, where filaments (prominences) are formed, are relative long-lived, narrow lanes between extended areas of magnetic field of opposite polarity. The channels are characterized by arcades of magnetic loops overlying an inner low-density cavity. The talk will review the observational bases, including small- to large-scale structure and dynamics, showing how filament channels differ from “normal” corona. One may subsequently understand better the conditions that lead to formation of filaments.
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Engvold, O. (1997). Filament Channels in the Corona. In: Mouradian, Z., Stavinschi, M. (eds) Theoretical and Observational Problems Related to Solar Eclipses. NATO ASI Series, vol 494. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-5492-5_22
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DOI: https://doi.org/10.1007/978-94-011-5492-5_22
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