A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament

	A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament
	Jiang, Chao-Wei; Wu, Shi-Tsan; Feng, Xue-Shang; Hu, Qiang
刊名	RESEARCH IN ASTRONOMY AND ASTROPHYSICS
	2016
卷号	16 期号:1 页码:18
关键词	magnetic fields Sun: corona Sun: filaments Sun: eruptions
ISSN号	1674-4527
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.
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.
收录类别	SCI
语种	英语
内容类型	期刊论文
源URL	[http://ir.nssc.ac.cn/handle/122/5664]
专题	国家空间科学中心_空间科学部
推荐引用方式 GB/T 7714	Jiang, Chao-Wei,Wu, Shi-Tsan,Feng, Xue-Shang,et al. A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament[J]. RESEARCH IN ASTRONOMY AND ASTROPHYSICS,2016,16(1):18.
APA	Jiang, Chao-Wei,Wu, Shi-Tsan,Feng, Xue-Shang,&Hu, Qiang.(2016).A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament.RESEARCH IN ASTRONOMY AND ASTROPHYSICS,16(1),18.
MLA	Jiang, Chao-Wei,et al."A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament".RESEARCH IN ASTRONOMY AND ASTROPHYSICS 16.1(2016):18.