Coronal Heating, Solar Filament Formation

Filament Channels: Isolated Laboratories of Plasma Heating in the Solar Corona

December 2015


Solar filament channels are complex systems comprising photospheric, chromospheric and coronal components. These components include magnetic neutral lines, supergranule cells, fibrils (spicules), filaments (prominences when observed on the limb), coronal cells, filament cavities and their overlying coronal arcades. Filaments are very highly structured and extend in height from the photosphere to the corona. Filament cores have chromospheric temperatures – 10,000 K (even at coronal heights ~ 100 Mm), surrounded by hotter plasma with temperature up to ~50,000 K. The whole filament is isolated from the rest of the solar corona by an envelope – the filament channel cavity – with temperatures of about 2,000,000 K. The filament channel cavity is even hotter than the solar corona outside the filament channel arcade. The compactness and big temperature variations make filament channels unique ready-to-go laboratories of coronal plasma heating and thermodynamics. In this work we discuss possible sources and mechanisms of heating in the filament channel environment. In particular, we address the mechanisms of magnetic canceling and current sheet dissipation.

Featured Publications

  2016 (1)
Rapid Reconnection and Field Line Topology. Parker, E.; and Rappazzo, A. In Gonzalez, W.; and Parker, E., editor(s), Astrophysics and Space Science Library, volume 427, pages 181, 2016.
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  2015 (1)
Observations and Analysis of the Non-Radial Propagation of Coronal Mass Ejections Near the Sun. Liewer, P.; Panasenco, O.; Vourlidas, A.; and Colaninno, R. \solphys, 290: 3343-3364. November 2015.
doi   bibtex
  2014 (1)
Apparent Solar Tornado-Like Prominences. Panasenco, O.; Martin, S.; and Velli, M. \solphys, 289: 603-622. February 2014.
doi   bibtex

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