Data-driven modeling of solar coronal magnetic field evolution and eruptions  

作　　者：Chaowei Jiang Xueshang Feng Yang Guo Qiang Hu 

机构地区：[1]Institute of Space Science and Applied Technology,Harbin Institute of Technology,Shenzhen 518055,China [2]School of Astronomy and Space Science,Nanjing University,Nanjing 210023,China [3]Department of Space Science,The University of Alabama in Huntsville,Huntsville,AL 35899,USA

出　　处：《The Innovation》2022年第3期27-41,共15页创新（英文）

基　　金：Thiswork is jointly supported by the National Natural Science Foundation of China(NSFC 42174200,41822404,and 41731067);the Fundamental Research Funds for the Central Universities(HIT.OCEF.2021033);the Shenzhen Science and Technology Program(RCJC20210609104422048 and JCYJ20190806142609035);Y.G.is supported by NSFC(11773016 and 11961131002)and 2020YFC2201201.We thank Dr.Aiying Duan for a careful reading of themanuscript.We are very grateful to the six reviewers for helpful comments and suggestions,which improved our manuscript.

摘　　要：Magnetic fields play a fundamental role in the structure and dynamics of the solar corona.As they are driven by their footpoint motions on the solar surface,which transport energy from the interior of the Sun into its atmosphere,the coronal magnetic fields are stressed continuously with buildup of magnetic nonpotentiality in the form of topology complexity(magnetic helicity)and local electric currents(magnetic free energy).The accumulated nonpotentiality is often released explosively by solar eruptions,manifested as solar flares and coronal mass ejections.

关 键 词：ERUPTION CORONAL EVOLUTION 

分 类 号：P18[天文地球—天文学]