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Abstract <p>Using two eruptive filaments as an example, it is shown that smooth axes of filaments can writhe into helical structures during eruption. This is a clear manifestation of kink instability, which, however, is not the trigger of eruption, but its result. The development of instability occurs at a late stage of eruption on a very large scale. This study is a continuation and development of work published earlier in The Astrophysical Journal, which focused only on the initial stage of eruption occurring at a relatively low height. To analyze the phenomena, observation data were used from the AIA (Atmospheric Imaging Assembly) and HMI (Heliospheric and Magnetic Imager) instruments on board SDO (Solar Dynamics Observatory), SECCHI EUVI (Sun Earth Connection Coronal and Heliospheric Investigation, Extreme UltraViolet Imager) on board STEREO (Solar Terrestrial Relations Observatory), LASCO C2 (Large Angle Spectrometric Coronagraph) on board SOHO (Solar and Heliospheric Observatory), as well as observations from ground-based telescopes. Comparison of images of filaments on the disk with calculations of the magnetic field in the corona gives a fairly reliable estimate of their initial height and convincingly indicates the proximity of the filaments to the threshold of eruptive instability, which probably causes eruptions as a result of the development of this instability. These examples contradict the fairly widespread opinion that kink instability usually initiates eruptions of magnetic flux ropes, and eruptive instability ensures their further development.</p>

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Writhing of the Axes of Eruptive Prominences at the Late Stage of Eruption

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  • 发表日期：

    2025年11月1日

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  • B. P. Filippov

摘要

Abstract

Using two eruptive filaments as an example, it is shown that smooth axes of filaments can writhe into helical structures during eruption. This is a clear manifestation of kink instability, which, however, is not the trigger of eruption, but its result. The development of instability occurs at a late stage of eruption on a very large scale. This study is a continuation and development of work published earlier in The Astrophysical Journal, which focused only on the initial stage of eruption occurring at a relatively low height. To analyze the phenomena, observation data were used from the AIA (Atmospheric Imaging Assembly) and HMI (Heliospheric and Magnetic Imager) instruments on board SDO (Solar Dynamics Observatory), SECCHI EUVI (Sun Earth Connection Coronal and Heliospheric Investigation, Extreme UltraViolet Imager) on board STEREO (Solar Terrestrial Relations Observatory), LASCO C2 (Large Angle Spectrometric Coronagraph) on board SOHO (Solar and Heliospheric Observatory), as well as observations from ground-based telescopes. Comparison of images of filaments on the disk with calculations of the magnetic field in the corona gives a fairly reliable estimate of their initial height and convincingly indicates the proximity of the filaments to the threshold of eruptive instability, which probably causes eruptions as a result of the development of this instability. These examples contradict the fairly widespread opinion that kink instability usually initiates eruptions of magnetic flux ropes, and eruptive instability ensures their further development.