Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels
文献类型：期刊论文
| 作者 | Li, Ting1; Zhang, Jun1; Ji, Haisheng2
|
| 刊名 | SOLAR PHYSICS
 |
| 出版日期 | 2015-06-01 |
| 卷号 | 290期号:6页码:1687-1702 |
| 关键词 | Prominences, formation and evolution Prominences, dynamics Magnetic fields, photosphere Coronal mass ejections, initiation and propagation |
| 英文摘要 | 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 -aEuro parts per thousand 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 6.4x10(21) 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 4.2x10(20) 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. |
| 学科主题 | 天文和天体物理 |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | Astronomy & Astrophysics |
| 关键词[WOS] | CORONAL MASS EJECTIONS ; CONFIGURATIONS SUPPORTING PROMINENCES ; DYNAMICS-OBSERVATORY SDO ; SOLAR ACTIVE REGIONS ; EMERGING FLUX ; H-ALPHA ; TRIGGER MECHANISM ; QUIET SUN ; ERUPTION ; FIELD |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000358068200010 |
| 源URL | [http://libir.pmo.ac.cn/handle/332002/14917]  |
| 专题 | 紫金山天文台_太阳活动的多波段观测研究团组 |
| 作者单位 | 1.Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China 2.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China |
| 推荐引用方式 GB/T 7714 | Li, Ting,Zhang, Jun,Ji, Haisheng. Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels[J]. SOLAR PHYSICS,2015,290(6):1687-1702. |
| APA | Li, Ting,Zhang, Jun,&Ji, Haisheng.(2015).Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels.SOLAR PHYSICS,290(6),1687-1702. |
| MLA | Li, Ting,et al."Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels".SOLAR PHYSICS 290.6(2015):1687-1702. |
入库方式： OAI收割
来源：紫金山天文台
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