The Evolution of Photospheric Current Density During an X9.3-Class Solar Flare  

作　　者：Hai-Li Li Hong-Fei Liang Xin-Ping Zhou Yu Liu Ni Meng Yu-Long Feng 

机构地区：[1]Department of Physics,Yunnan Normal University,Kunming 650500,China [2]State Key Laboratory of Space Weather,Chinese Academy of Sciences,Beijing 100190,China [3]College of Physics and Electronic Engineering,Sichuan Normal University,Chengdu 610068,China [4]School of Physical Science and Technology,Southwest Jiaotong University,Chengdu 610068,China

出　　处：《Research in Astronomy and Astrophysics》2024年第10期189-200,共12页天文和天体物理学研究（英文版）

基　　金：supported by the Natural Natural Science Foundation of China(NSFC,grant No.12303062);Sichuan Science and Technology Program(2023NSFSC1351);Joint Funds of the National Natural Science Foundation of China(NSFC,grant No.U1931116);the Project Supported by the Specialized Research Fund for State Key Laboratories。

摘　　要：This paper deduced the temporal evolution of the magnetic field through a series of high-resolution vector magnetograms and calculated the fine distribution map of current density during an X9.3-class flare eruptions using Ampère's law.The results show that a pair of conjugate current ribbons exist on both sides of the magnetic neutral line in this active region,and these conjugate current ribbons persist before,during,and after the flare.It was observed that the X9.3-class flare brightened in the form of a bright core and evolved into a double-ribbon flare over time.Importantly,the position of the double-ribbon flare matches the position of the current ribbons with high accuracy,and their morphologies are very similar.By investigating the complexity of current density and flare morphology,we discovered a potential connection between the eruption of major flares and the characteristics of current density.

关 键 词：Sun:activity Sun:magnetic fields Sun:flares methods:data analysis 

分 类 号：P182.52[天文地球—天文学]