PMO OpenIR  > 太阳活动的多波段观测研究团组
Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog
McCauley, PI; Su, YN; Schanche, N; Evans, KE; Su, C; McKillop, S; Reeves, KK
2015
Source PublicationSOLAR PHYSICS
Volume290Issue:6Pages:1703-1740
AbstractWe 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.
Subject Area天文和天体物理
Indexed BySCI
Language英语
WOS IDWOS:000358068200011
Citation statistics
Cited Times:52[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/14918
Collection太阳活动的多波段观测研究团组
Recommended Citation
GB/T 7714
McCauley, PI,Su, YN,Schanche, N,et al. Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog[J]. SOLAR PHYSICS,2015,290(6):1703-1740.
APA McCauley, PI.,Su, YN.,Schanche, N.,Evans, KE.,Su, C.,...&Reeves, KK.(2015).Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog.SOLAR PHYSICS,290(6),1703-1740.
MLA McCauley, PI,et al."Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog".SOLAR PHYSICS 290.6(2015):1703-1740.
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