Breaking of Large-Scale Filament due to Magnetic Reconnection and Consequent Partial Eruption  

作　　者：Kaifeng Kang Yang Guo Yan Li Jingxing Wang Jun Lin 

机构地区：[1]Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China [2]University of Chinese Academy of Sciences,Beijing 100049,China [3]Center for Astronomical Mega-Science,Chinese Academy of Sciences,Beijing 100101,China [4]Yunnan Key Laboratory of Solar Physics and Space Science,Kunming 650216,China [5]School of Astronomy and Space Science and Key Laboratory for Modern Astronomy and Astrophysics,Nanjing University,Nanjing 210023,China

出　　处：《Research in Astronomy and Astrophysics》2023年第9期194-206,共13页天文和天体物理学研究（英文版）

基　　金：supported by the National Key R&D Program of China No.2022YFF0503804;the Strategic Priority Research Programme of the Chinese Academy of Sciences with grant XDA17040507;the National Natural Science Foundation of China (NSFC) grant 11 933 009;grants associated with the Yunling Scholar Project of Yunnan Province,the Yunnan Province Scientist Workshop of Solar Physics.

摘　　要：Following our previous work,we studied the partial eruption of a large-scale horse-shoe-like filament that had beenobserved in a decaying active region on the solar disk for more than 4.5 days.The filament became active after itwas broken into two pieces,P1 and P2 seen in Hα,by magnetic reconnection between the magnetic field around itand that of a newly emerging active region nearby.P1 eventually erupted 13 hr after the breaking and escaped fromthe Sun,developing to a fast coronal mass ejection,and P2 stayed.But the mass in P1 falling down to P2 in theeruption suggests that the global magnetic fields over P1 and P2 were still connected to each other prior to theeruption.The reconnection process breaking the filament occurred outside the filament,and P1 and P2 were locatedalmost at the same altitude,so the fashion of the filament partial eruption studied here differs from that of the“double-decker model”and that of reconnection inside the filament.Analyzing the decay indices of thebackground fields above P1 and P2,n_(1)and n_(2),showed that the altitude where n_(1)exceeds the critical value of n_(c)=1.5 for the loss of equilibrium or the torus instability is lower than that where n_(2)>nc,and that n_(1)>n_(2) alwaysholds at all altitudes.Combining this fact with that the eruption occurred 13 hr after filament was broken byreconnection,we conclude that the eruption of P1 was triggered by the loss of equilibrium or the torus instability inthe configuration,and magnetic reconnection breaking the filament helped weaken the confinement of thebackground field on P1,allowing P1 to erupt.Detailed features of the eruption and the corresponding physicalscenario were also discussed.

关 键 词：SUN activity-Sun filaments-prominences-Sun coronal mass ejections(CMEs)-Sun flares-Sun magnetic fields 

分 类 号：P182[天文地球—天文学]