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Spike emission at 21 cm wavelength in post-flare loops

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Abstract

Electron-cyclotron maser instability produced by accelerated energetic electrons is today's most favoured process for spike emission on ultra-short time scales at dm wavelengths. The process of electron acceleration occurs primarily in pre-impulsive and impulsive phases. We present observations of spike bursts at 21 cm in a limb event that occurred in AR 5629 on 1989 August 17. Optical observations of the event from Beijing Astronomical Observatory show coronal loops that interact just before the spike groups appeared. This implies that additional particle acceleration might be produced by the interaction between emerging loops and original large loops, and become the source of the energetic electrons responsible for the spike emission appearing in the descending phase. Some important parameters are deduced.

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Authors and Affiliations

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

    Fu Qijun, Li Wei & Zhao Bing

  2. Department of Astronomy, Nanjing University, 210008, Nanjing, China (NJU)

    Li Chunsheng

  3. Yunnan Astronomical Observatory, Chinese Academy of Sciences, 650011, Kunming, China (YAO)

    Gong Yuanfang, Shang Qiongzhen, Lu Songquan & Hu Hanming

Authors
  1. Fu Qijun
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  2. Li Chunsheng
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  3. Gong Yuanfang
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  4. Li Wei
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  5. Zhao Bing
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  6. Shang Qiongzhen
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  7. Lu Songquan
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  8. Hu Hanming
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Fu, Q., Li, C., Gong, Y. et al. Spike emission at 21 cm wavelength in post-flare loops. Sol Phys 143, 317–326 (1993). https://doi.org/10.1007/BF00646490

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  • DOI: https://doi.org/10.1007/BF00646490

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