Magnetic causes of the eruption of a quiescent filament

CORC > 紫金山天文台 > 中国科学院紫金山天文台 > 太阳高能及相关物理过程研究团组

	Magnetic causes of the eruption of a quiescent filament
	Schmieder, B.1; Bommier, V.2; Kitai, R.3; Matsumoto, T.3; Ishii, T. T.3; Hagino, M.3; Li, H.4 ; Golub, L.5
刊名	SOLAR PHYSICS
	2008-02-01
卷号	247 期号:2 页码:321-333
关键词	Sun filament eruption magnetic field
ISSN号	0038-0938
英文摘要	During the JOP178 campaign in August 2006, we observed the disappearance of our target, a large quiescent filament located at S25, after an observation time of three days ( 24 August to 26 August). Multi-wavelength instruments were operating: THEMIS/MTR ("MulTi-Raies") vector magnetograph, TRACE ("Transition Region and Coronal Explorer") at 171 angstrom and 1600 angstrom and Hida Domeless Solar telescope. Counter-streaming flows (+/- 10 kms(-1)) in the filament were detected more than 24 hours before its eruption. A slow rise of the global structure started during this time period with a velocity estimated to be of the order of 1 kms(-1). During the hour before the eruption ( 26 August around 09: 00 UT) the velocity reached 5 kms(-1). The filament eruption is suspected to be responsible for a slow CME observed by LASCO around 21: 00 UT on 26 August. No brightening in H alpha or in coronal lines, no new emerging polarities in the filament channel, even with the high polarimetry sensitivity of THEMIS, were detected. We measured a relatively large decrease of the photospheric magnetic field strength of the network ( from 400 G to 100 G), whose downward magnetic tension provides stability to the underlying stressed filament magnetic fields. According to some MHD models based on turbulent photospheric diffusion, this gentle decrease of magnetic strength (the tension) could act as the destabilizing mechanism which first leads to the slow filament rise and its fast eruption.
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]	CORONAL MASS EJECTIONS ; TRANSITION REGION ; FLUX ROPE ; PROMINENCES ; FLOWS ; MODEL ; MULTIWAVELENGTH ; EVOLUTION ; EXPLORER ; FLARES
收录类别	SCI
语种	英语
WOS记录号	WOS:000252946200006
公开日期	2011-12-29
内容类型	期刊论文
源URL	[http://159.226.72.40/handle/332002/1877]
专题	紫金山天文台_太阳高能及相关物理过程研究团组
作者单位	1.CNRS, UMR 8109, LESIA, Observ Paris, F-92195 Meudon, France 2.CNRS, UMR 8112, LERMA, Observ Paris, F-92195 Meudon, France 3.Kyoto Univ, Hida Observ, Kyoto, Japan 4.Purple Mountain Observ, Nanjing 210008, Peoples R China 5.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
推荐引用方式 GB/T 7714	Schmieder, B.,Bommier, V.,Kitai, R.,et al. Magnetic causes of the eruption of a quiescent filament[J]. SOLAR PHYSICS,2008,247(2):321-333.
APA	Schmieder, B..,Bommier, V..,Kitai, R..,Matsumoto, T..,Ishii, T. T..,...&Golub, L..(2008).Magnetic causes of the eruption of a quiescent filament.SOLAR PHYSICS,247(2),321-333.
MLA	Schmieder, B.,et al."Magnetic causes of the eruption of a quiescent filament".SOLAR PHYSICS 247.2(2008):321-333.