Solar Physics

, Volume 291, Issue 8, pp 2373–2390 | Cite as

An Observational Study of the Recurring Formation and Dissipation of a Dynamic Filament

  • Guiping ZhouEmail author
  • Jingxiu Wang
  • Jie Zhang


Based on observations at the \(\mbox{H}\upalpha\) wavelength from the Hinode spacecraft, we report here the detailed process of a dynamical filament that showed repeated appearance and dissipation in a filament channel. First, \(\mbox{H}\upalpha\) short fibrils spreading in the pre-formed filament channel joined into longer threads. The joining process was found to be accompanied by small-scale brightening activity, indicating the possible involvement of magnetic reconnection. The forming filament was thickened by merging the neighboring dark threads that were nearly parallel to the axis and also those adjacent to its main endpoints. The formed filament as a single coherent structure only existed for tens of minutes, immediately followed by the dissipation. The dissipation appeared to start with expansion of the filament body, ascending and stripping away of the filament threads, and mass drainage along the legs of the filament. The formation–dissipation process of the filament was repeated three times within the four-hour observational window of Hinode. These observations indicate that the filament structure is highly dynamic. This study provides the observational evidence to confirm the hypothesis of Martin et al. (Ann. Geophys. 26, 3061, 2008) on the irreversible build-up of magnetic fields in the corona by discrete threads or groups of threads ascending bodily into the corona.


Prominences, Formation and Evolution Corona, Structures Magnetic fields, Photosphere 



We sincerely thank Saku Tsuneta for his very helpful suggestions and discussions. We are deeply grateful to the anonymous referee for many insightful and valuable suggestions that significantly improved the quality of the article. We thank all members of Hinode teams for providing the wonderful data. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. The work is supported by the National Natural Science Foundation of China (11322329, 10973019, 11533008, 11573038, and 11303049), the National Key Basic Research Science Foundation (G2011CB811402), and the Open Research Program of Key Laboratory of Solar Activity, National Astronomical Observatories of China (KLSA201416). J. Zhang is supported by NSF AGS-1156120 and NSF AGS-1249270.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

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Authors and Affiliations

  1. 1.Key Laboratory of Solar Activity, National Astronomical ObservatoriesChinese Academy of ScienceBeijingChina
  2. 2.School of Physics, Astronomy and Computational SciencesGeorge Mason UniversityFairfaxUSA

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