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

ISSN号：1674-4527
期刊名称：Research in Astronomy and Astrophysics
时间：2011.6.6
页码：692-700
分类：P182.52[天文地球—天文学] P318.2[天文地球—固体地球物理学;天文地球—地球物理学]
作者机构：[1]epartment of Astronomy,Nanjing University,Nanjing 210093,China, [2]Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210008,China, [3]Space Weather Research Lab,Center for Solar Terrestrial Research,New Jersey Institute of Technology,Newark,NJ 07102,US
相关基金：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
相关项目：太阳活动在不同层次的特征和耦合

作者： Wang, Pu|Ding, Ming-De|Ji, Hai-Sheng|Wang, Hai-Min|

关键词：太阳耀斑, 磁场变化, M级, 观测数据, 磁通量, IVM, NOAA, 时间演化, Sun：activity-Sun：magnetic field-Sun：flares

中文摘要：

与广泛的分析，我们在二个邻近的活跃区域在三连续 M 班闪光期间学习磁性的流动的时间的进化：NOAA 10039 并且 10044。主要数据是纵的 magnetograms 由 SOHO/MDI 观察了的完整的磁盘。所有三闪光被观察被磁性的流动变化伴随。变化立即或在 10 在闪光的开始的时间以后纪录的 1 ~ 以内发生了，显示变化是太阳耀斑的明显的后果。尽管在许多点的变化在磁性的流动是内在的，为一些地点，它被磁性的流动的一个快速的扩大运动引起。为第二闪光，联系变化与“步功能”相比是更渐渐的在文学报导了。而且，我们使用成像向量磁针自记仪(IVM ) 在 Mees 太阳的天文台观察在闪光期间检查可能的线侧面变化的数据。从 IVM 数据的结果证实从 MDI 数据获得的流动变化。一系列线侧面从 IVM 的观察被获得并且为流动变化地点分析了。我们发现在宽度，深度和线的中央波长的变化甚至在闪光的核心是不到 5.0% 。没有线侧面变化被观察在期间或在闪光以后。我们断定与三个太阳耀斑联系的磁场变化没被闪光排放引起。

英文摘要：

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 10044.The primary data are full disk longitudinal magnetograms observed by SOHO/MDI.All three flares are observed to be accompanied by magnetic flux changes.The 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 flares.Although changes in many points are intrinsic in magnetic flux,for some sites,it is caused by a rapid expansion motion of magnetic flux.For the second flare,the associated change is more gradual compared with the ＇step-function＇ reported in literature.Furthermore,we use the data observed by the Imaging Vector Magnetograph（IVM） at Mees Solar Observatory to check possible line profile changes during the flares.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 sites.We find that the fluctuations in the width,depth and central wavelength of the lines are less than 5.0 even at the flare＇s core.No line profile change is observed during or after the flare.We conclude that the magnetic field changes associated with the three solar flares are not caused by flare emission.

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