Coupling of small-and large-scale filament eruptions  

作　　者：Jia-Yan Yang Yun-Chun Jiang Bo Yang Jun-Chao Hong Zhe Xu 

机构地区：[1]Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China [2]University of Chinese Academy of Sciences, Beijing 100049, China

出　　处：《Research in Astronomy and Astrophysics》2016年第1期23-30,共8页天文和天体物理学研究（英文版）

基　　金：supported by the National Natural Science Foundation of China (NSFC,Grant Nos.11273056,11473065 and 11333007)

摘　　要：We present observations of the eruption of a large-scale quiescent filament （LF） that is associated with the formation and eruption of a miniature filament （MF）. As a result of convergence and subsequent cancelation of opposite-polarity magnetic flux, MF was formed just below the spine of the LF＇s right seg- ment. Probably triggered by a nearby newly emerging flux, MF underwent a failed eruption immediately after its full development, which first ejected away from the spine of LF and then drained back to the Sun. This eruption no sooner started than the overlying LF＇s right segment began to rise slowly and the LF＇s other parts were also disturbed, and eventually the whole LF erupted bodily and quickly. These observa- tions suggest that the MF can serve as an intermediary that links the photospheric small-scale magnetic-field activities to the eruption of the overlying large filament. It appears that, rather than directly interacting with the supporting magnetic field of LF, small-scale flux cancelation and emergence in the LF＇s channel can manifest themselves as the formation and eruption of MF and so indirectly affect the stability of LEWe present observations of the eruption of a large-scale quiescent filament （LF） that is associated with the formation and eruption of a miniature filament （MF）. As a result of convergence and subsequent cancelation of opposite-polarity magnetic flux, MF was formed just below the spine of the LF＇s right seg- ment. Probably triggered by a nearby newly emerging flux, MF underwent a failed eruption immediately after its full development, which first ejected away from the spine of LF and then drained back to the Sun. This eruption no sooner started than the overlying LF＇s right segment began to rise slowly and the LF＇s other parts were also disturbed, and eventually the whole LF erupted bodily and quickly. These observa- tions suggest that the MF can serve as an intermediary that links the photospheric small-scale magnetic-field activities to the eruption of the overlying large filament. It appears that, rather than directly interacting with the supporting magnetic field of LF, small-scale flux cancelation and emergence in the LF＇s channel can manifest themselves as the formation and eruption of MF and so indirectly affect the stability of LE

关 键 词：Sun： activity -- Sun： filaments -- Sun： magnetic fields 

分 类 号：P182[天文地球—天文学]