Magnetic field changes associated with three successive M-class solar flares on 2002 July 26

作     者：Pu Wang Ming-De Ding Hai-Sheng Ji Hai-Min Wang 

作者机构：epartment of AstronomyNanjing UniversityNanjing 210093China Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210008China Space Weather Research LabCenter for Solar Terrestrial ResearchNew Jersey Institute of TechnologyNewarkNJ 07102US 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2011年第11卷第6期

页      面：692-700页

核心收录：

学科分类：070801[理学-固体地球物理学] 07[理学] 0708[理学-地球物理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：Supported by the National Natural Science Foundation of China (Grants Nos. 10833007,10933003 and 10928307) the National Basic Research Program of China (973 Program) under grant 2011CB811402 

主　　题：Sun:activity Sun:magnetic field Sun:flares 

摘      要：With an extensive analysis,we study the temporal evolution of magnetic flux during three successive M-class flares in two adjacent active regions：NOAA 10039 and *** primary data are full disk longitudinal magnetograms observed by SOHO/*** three flares are observed to be accompanied by magnetic flux *** changes occurred immediately or within 1 ～ 10 minutes after the starting time of the flares,indicating that the changes are obvious consequences of the solar *** changes in many points are intrinsic in magnetic flux,for some sites,it is caused by a rapid expansion motion of magnetic *** the second flare,the associated change is more gradual compared with the ＇step-function＇ reported in ***,we use the data observed by the Imaging Vector Magnetograph（IVM） at Mees Solar Observatory to check possible line profile changes during the *** results from the IVM data confirm the flux changes obtained from the MDI data.A series of line profiles were obtained from the IVM＇s observations and analyzed for flux change *** find that the fluctuations in the width,depth and central wavelength of the lines are less than 5.0 even at the flare＇s *** line profile change is observed during or after the *** conclude that the magnetic field changes associated with the three solar flares are not caused by flare emission.