Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels
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- 作者：Ting Li ; Jun Zhang ; Haisheng Ji
- 关键词：Prominences ; formation and evolution ; Prominences ; dynamics ; Magnetic fields ; photosphere ; Coronal mass ejections ; initiation and propagation
- 刊名：Solar Physics
- 出版年：2015
- 出版时间：June 2015
- 年：2015
- 卷：290
- 期：6
- 页码：1687-1702
- 全文大小：4,006 KB
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Scherrer, P.H., Schou, J., Bush, R.I., Kosovichev, A.G., Bogart, R.S., Hoeksema, J.T., e - 作者单位：Ting Li (1)
Jun Zhang (1)
Haisheng Ji (2)
1. Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China
2. Key Laboratory for Dark Matter and Space Science, Purple Mountain Observatory, CAS, Nanjing, 210008, China - 刊物类别：Physics and Astronomy
- 刊物主题：Physics
Astronomy
Extraterrestrial Physics and Space Sciences
Astrophysics - 出版者：Springer Netherlands
- ISSN：1573-093X
文摘
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?–-0 (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.