3D magnetic field configuration of the 2006 December 13 flare extrapolated with the optimization method

CORC > 紫金山天文台 > 中国科学院紫金山天文台 > 星系中的恒星形成研究团组

	3D magnetic field configuration of the 2006 December 13 flare extrapolated with the optimization method
	Guo, Y.1; Ding, M. D.1; Wiegelmann, T.2; Li, H.3
刊名	ASTROPHYSICAL JOURNAL
	2008-06-01
卷号	679 期号:2 页码:1629-1635
关键词	Sun : flares Sun : magnetic fields
ISSN号	0004-637X
英文摘要	The photospheric vector magnetic field of the active region NOAA 10930 was obtained with the Solar Optical Telescope (SOT) on board the Hinode satellite with a very high spatial resolution (about 0.3 ''). Observations of the two-ribbon flare on 2006 December 13 in this active region provide us a good sample to study the magnetic field configuration related to the occurrence of the flare. Using the optimization method for nonlinear force-free field (NLFFF) extrapolation proposed by Wheatland et al. and recently developed by Wiegelmann, we derive the three-dimensional (3D) vector magnetic field configuration associated with this flare. The general topology can be described as a highly sheared core field and a quasi-potential envelope arch field. The core field clearly shows some dips supposed to sustain a filament. Free energy release in the flare, calculated by subtracting the energy contained in the NLFFF and the corresponding potential field, is 2: 4; 1031 ergs, which is similar to 2% of the preflare potential field energy. We also calculate the shear angles, defined as the angles between the NLFFF and potential field, and find that they become larger at some particular sites in the lower atmosphere, while they become significantly smaller in most places, implying that the whole configuration gets closer to the potential field after the flare. The Ca II H line images obtained with the Broadband Filter Imager (BFI) of the SOT and the 1600 8 images with the Transition Region and Coronal Explorer (TRACE) show that the preflare heating occurs mainly in the core field. These results provide evidence in support of the tether-cutting model of solar flares.
学科主题	Astronomy & Astrophysics
WOS标题词	Science & Technology ; Physical Sciences
类目[WOS]	Astronomy & Astrophysics
研究领域[WOS]	Astronomy & Astrophysics
关键词[WOS]	FORCE-FREE FIELDS ; CORONAL MASS EJECTIONS ; SOLAR ACTIVE-REGION ; BOUNDARY DATA ; RECONSTRUCTION ; CANCELLATION ; AMBIGUITY ; ERUPTION ; EVENT
收录类别	SCI
语种	英语
WOS记录号	WOS:000256315500056
公开日期	2011-12-29
内容类型	期刊论文
源URL	[http://159.226.72.40/handle/332002/1921]
专题	紫金山天文台_星系中的恒星形成研究团组
作者单位	1.Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China 2.Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany 3.Purple Mt Observ, Nanjing 210008, Peoples R China
推荐引用方式 GB/T 7714	Guo, Y.,Ding, M. D.,Wiegelmann, T.,et al. 3D magnetic field configuration of the 2006 December 13 flare extrapolated with the optimization method[J]. ASTROPHYSICAL JOURNAL,2008,679(2):1629-1635.
APA	Guo, Y.,Ding, M. D.,Wiegelmann, T.,&Li, H..(2008).3D magnetic field configuration of the 2006 December 13 flare extrapolated with the optimization method.ASTROPHYSICAL JOURNAL,679(2),1629-1635.
MLA	Guo, Y.,et al."3D magnetic field configuration of the 2006 December 13 flare extrapolated with the optimization method".ASTROPHYSICAL JOURNAL 679.2(2008):1629-1635.