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题名: A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament
作者: Jiang, Chao-Wei; Wu, Shi-Tsan; Feng, Xue-Shang; Hu, Qiang
作者部门: 空间科学部
通讯作者: Jiang, CW (reprint author), Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, SIGMA Weather Grp, Beijing 100190, Peoples R China.
关键词: magnetic fields ; Sun: corona ; Sun: filaments ; Sun: eruptions
刊名: RESEARCH IN ASTRONOMY AND ASTROPHYSICS
ISSN号: 1674-4527
出版日期: 2016
卷号: 16, 期号:1, 页码:18
收录类别: SCI
项目资助者: 973 program [2012CB825601] ; Chinese Academy of Sciences [KZZD-EW-01-4] ; National Natural Science Foundation of China [41204126, 41231068, 41274192, 41031066, 41374176] ; Specialized Research Fund for State Key Laboratories ; Youth Innovation Promotion Association of CAS [2015122] ; [NSF-AGS1153323] ; [AGS1062050]
英文摘要: Solar active region (AR) 11283 is a very magnetically complex region and it has produced many eruptions. However, there exists a non-eruptive filament in the plage region just next to an eruptive one in the AR, which gives us an opportunity to perform a comparison analysis of these two filaments. The coronal magnetic field extrapolated using our CESE-MHD-NLFFF code reveals that two magnetic flux ropes (MFRs) exist in the same extrapolation box supporting these two filaments, respectively. Analysis of the magnetic field shows that the eruptive MFR contains a bald-patch separatrix surface (BPSS) cospatial very well with a pre-eruptive EUV sigmoid, which is consistent with the BPSS model for coronal sigmoids. The magnetic dips of the non-eruptive MFRs match H alpha observation of the non-eruptive filament strikingly well, which strongly supports the MFR-dip model for filaments. Compared with the non-eruptive MFR/filament (with a length of about 200 Mm), the eruptive MFR/filament is much smaller (with a length of about 20Mm), but it contains most of the magnetic free energy in the extrapolation box and holds a much higher free energy density than the non-eruptive one. Both the MFRs are weakly twisted and cannot trigger kink instability. The AR eruptive MFR is unstable because its axis reaches above a critical height for torus instability, at which the overlying closed arcades can no longer confine the MFR stably. On the contrary, the quiescent MFR is very firmly held by its overlying field, as its axis apex is far below the torus-instability threshold height. Overall, this comparison investigation supports that an MFR can exist prior to eruption and the ideal MHD instability can trigger an MFR eruption.
语种: 英语
内容类型: 期刊论文
URI标识: http://ir.nssc.ac.cn/handle/122/5664
Appears in Collections:空间科学部_期刊论文

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