PMO OpenIR  > 太阳活动的多波段观测研究团组
Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels
Li, Ting1; Zhang, Jun1; Ji, Haisheng2
2015-06-01
Source PublicationSOLAR PHYSICS
Volume290Issue:6Pages:1687-1702
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.
KeywordProminences, Formation And Evolution Prominences, Dynamics Magnetic Fields, Photosphere Coronal Mass Ejections, Initiation And Propagation
Subject Area天文和天体物理
WOS HeadingsScience & Technology ; Physical Sciences
DOI10.1007/s11207-015-0698-8
WOS KeywordCORONAL MASS EJECTIONS ; CONFIGURATIONS SUPPORTING PROMINENCES ; DYNAMICS-OBSERVATORY SDO ; SOLAR ACTIVE REGIONS ; EMERGING FLUX ; H-ALPHA ; TRIGGER MECHANISM ; QUIET SUN ; ERUPTION ; FIELD
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000358068200010
Citation statistics
Cited Times:6[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/14917
Collection太阳活动的多波段观测研究团组
Affiliation1.Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China
2.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China
Recommended Citation
GB/T 7714
Li, Ting,Zhang, Jun,Ji, Haisheng. Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels[J]. SOLAR PHYSICS,2015,290(6):1687-1702.
APA Li, Ting,Zhang, Jun,&Ji, Haisheng.(2015).Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels.SOLAR PHYSICS,290(6),1687-1702.
MLA Li, Ting,et al."Filament Activation in Response to Magnetic Flux Emergence and Cancellation in Filament Channels".SOLAR PHYSICS 290.6(2015):1687-1702.
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