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Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels

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Abstract

We conducted a comparative analysis of two filaments that showed a quite different activation in response to the flux emergence within the filament channels. The observations from the Solar Dynamics Observatory (SDO) and Global Oscillation Network Group (GONG) were made to analyze the two filaments on 2013 August 17 – 20 (SOL2013-08-17) and September 29 (SOL2013-09-29). The first event showed that the main body of the filament was separated into two parts when an active region (AR) emerged with a maximum magnetic flux of about 6.4×1021 Mx underlying the filament. The close neighborhood and common direction of the bright threads in the filament and the open AR fan loops suggest a similar magnetic connectivity of these two flux systems. The equilibrium of the filament was not destroyed three days after the start of the emergence of the AR. To our knowledge, similar observations have never been reported before. In the second event, the emerging flux occurred nearby a barb of the filament with a maximum magnetic flux of 4.2×1020 Mx, about one order of magnitude lower than that of the first event. Two patches of parasitic polarity in the vicinity of the barb merged, then cancelled with nearby network fields. About 20 hours after the onset of the emergence, the filament erupted. Our findings imply that the location of emerging flux within the filament channel is probably crucial to filament evolution. If the flux emergence appears nearby the barbs, it is highly likely that the emerging flux and the filament magnetic fields will cancel, which may lead to the eruption of the filament. The comparison of the two events shows that the emergence of a small AR may still not be enough to disrupt the stability of a filament system, and the actual eruption only occurs after the flux cancellation sets in.

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Acknowledgements

We acknowledge the SDO/AIA, HMI, and NSO–GONG for providing data. This work is supported by the National Basic Research Program of China under grant 2011CB811403, the National Natural Science Foundations of China (11303050, 11025315, 11221063 and 11003026), the CAS Project KJCX2-EW-T07 and the Strategic Priority Research Program – The Emergence of Cosmological Structures of the Chinese Academy of Sciences, Grant No. XDB09000000. H.S. Ji was supported by NSFC grants 11333009 and 1117306.

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  1. Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China

    Ting Li & Jun Zhang

  2. Key Laboratory for Dark Matter and Space Science, Purple Mountain Observatory, CAS, Nanjing, 210008, China

    Haisheng Ji

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  1. Ting Li
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Correspondence to Ting Li.

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Li, T., Zhang, J. & Ji, H. Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels. Sol Phys 290, 1687–1702 (2015). https://doi.org/10.1007/s11207-015-0698-8

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