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Structures of chromospheric magnetic field in the vicinity of the filament of active region 5669

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Abstract

In this paper, the chromospheric magnetic structures and their relation to the photospheric vector magnetic field in the vicinity of a dark filament in active region 5669 have been demonstrated. Structural variations are shown in chromospheric magnetograms after a solar flare. Filament-like structures in the chromospheric magnetograms occurred after a solar flare. They correspond to the reformation of the chromospheric dark filament, but there is no obvious variation of the photospheric magnetic field. We conclude that (a) some of the obvious changes of the chromospheric magnetic fields occurred after the flare, and (b) a part of these changes is perhaps due to flare brightening in the chromospheric Hβ line.

During the reforming process of the dark filament, a part of its chromospheric velocity field shows downward flow, and it later shows upward flow.

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Authors and Affiliations

  1. Beijing Astronomical Observatory, Chinese Academy of Sciences, 100080, Beijing, China

    Hongqi Zhang, Guoxiang Ai, Wei Li & Jimin Chen

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  1. Hongqi Zhang
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  2. Guoxiang Ai
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  3. Wei Li
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  4. Jimin Chen
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Zhang, H., Ai, G., Li, W. et al. Structures of chromospheric magnetic field in the vicinity of the filament of active region 5669. Sol Phys 146, 61–74 (1993). https://doi.org/10.1007/BF00662170

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  • DOI: https://doi.org/10.1007/BF00662170

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