Consecutive narrow and broad quasi-periodic fast-propagating wave trains associated with a flare  

作　　者：Xinping Zhou Yuandeng Shen Chengrui Zhou Zehao Tang Ahmed Ahmed Ibrahim 

机构地区：[1]College of Physics and Electronic Engineering,Sichuan Normal University,Chengdu 610068,China [2]State Key Laboratory of Space Weather,Chinese Academy of Sciences,Beijing 100190,China [3]Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China [4]Department of Physics and Astronomy,College of Science,King Saud University,P.O.Box 2455,Riyadh 11451,Saudi Arabia

出　　处：《Science China(Physics,Mechanics & Astronomy)》2024年第5期200-211,共12页中国科学：物理学、力学、天文学（英文版）

基　　金：supported by the National Natural Science Foundation of China(Grant No.12303062);the Natural Science Foundation for Youths of Sichuan Province(Grant No.2023NSFSC1351);the Project Supported by the Specialized Research Fund for State Key Laboratories;supported by the National Natural Science Foundation of China(Grant No.12173083);the Yunnan Science Foundation for Distinguished Young Scholars(Grant No.202101AV070004);the Researchers Supporting Project(Grant Nos.RSPD2023R993,and RSPD2024R993),King Saud University,Riyadh,Saudi Arabia;ISSI-BJ for supporting the international team“Magnetohydrodynamic wave trains as a tool for probing the solar corona”。

摘　　要：The excitation mechanism of coronal quasi-period fast-propagating(QFP)wave trains remains unresolved.Using Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory observations,we study a narrow and a broad QFP wave trains excited one after another during the successive eruptions of filaments hosted within a fan-spine magnetic system on October 20,2013.The consecutive occurrence of these two types of QFP wave trains in the same event provides an excellent opportunity to explore their excitation mechanisms and compare their physical parameters.Our observational results reveal that narrow and broad QFP wave trains exhibit distinct speeds,periods,energy fluxes,and relative intensity amplitudes,although originating from the same active region and being associated with the same GOES C2.9 flare.Using wavelet analysis,we find that the narrow QFP wave train shares a similar period with the flare itself,suggesting its possible excitation through the pulsed energy release in the magnetic reconnection process that generated the accompanying flare.On the other hand,the broad QFP wave train appears to be associated with the energy pulses released by the successive expansion and unwinding of filament threads.Additionally,it is plausible that the broad QFP wave train was also excited by the sequential stretching of closed magnetic field lines driven by the erupting filament.These findings shed light on the different excitation mechanisms and origins of the QFP wave trains.

关 键 词：NARROW wave EXCITATION 

分 类 号：P182.52[天文地球—天文学]