Large-scale activity in solar eruptive events of October–November 2003 observed from SOHO/EIT data
Large-scale activity in solar eruptive events of October–November 2003 observed from SOHO/EIT data
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DOI：
10.1134/1.1862362
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发表时间：
2005-02
影响因子：
1
通讯作者：
I. Chertok;V. Grechnev
中科院分区：
文献类型：
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作者：
I. Chertok;V. Grechnev
利用SOHO/EIT极紫外望远镜观测的数据，分析了2003年11月至2004年11月期间，在一个由三个活动区组成的大系统的两次通过期间，与强耀斑和日冕物质抛射（CME）相关的大尺度太阳扰动。调光（瞬态日冕洞），并在较小程度上，日冕波（旅行发射锋）研究使用固定的差异去旋图像，其中应用的太阳旋转校正和一个单一的日光图之前的事件是从所有后续的日光图减去。这种方法使我们能够研究195 Å线（间隔12分钟）和171、195、284和304 Å不同温度通道（间隔6小时）的差异日光图。我们的分析表明，特别是，与CME的扰动表现出全球性的特点，几乎占据了整个南半部的磁盘在几乎所有的爆发事件在两个太阳旋转。与此同时，圆盘的北方有一个巨大的冕洞，只是受到轻微的干扰。在盘面上观察到的主要变暗是狭长的特征，主要分布在系统的三个主要的、分离良好的区域之间，以及位于南极扇区太阳纬度沿着的长结构。对于间隔时间不长的重复事件，其主导调光在形式和位置上表现出明显的同源性。在10月28日的非常强大的事件中，一个相应的全球变暗集合变成了另一个集合。在三个日冕通道和过渡区线中观察到许多相同或非常相似的暗化。分析表明，日冕和过渡区快速恢复的全球结构与运行中的日冕物质抛射的爆发和相应的大尺度磁场重建有关。
Large-scale solar disturbances associated with powerful flares and coronal mass ejections (CMEs) during two passages of a grand system of three active regions in October–November 2003 are analyzed using data obtained with the SOHO/EIT EUV telescope. Dimmings (transient coronal holes) and, to a lesser extent, coronal waves (traveling emitting fronts) are studied using fixed-difference derotated images, in which a correction for the solar rotation is applied and a single heliogram preceding the event is subtracted from all subsequent heliograms. This method allows us to study difference heliograms in both the 195 Å line (with an interval of 12 min) and the various-temperature channels of 171, 195, 284, and 304 Å (with an interval of six hours). Our analysis shows, in particular, that the disturbances associated with CMEs demonstrated a global character and occupied almost the entire southern half of the disk in virtually all eruptive events during the two solar rotations. At the same time, the northern half of the disk, which had a large coronal hole, was only slightly disturbed. The dominant dimmings were observed on the disk as narrow, long features stretched mainly between three main, well-separated regions of the system and as long structures located along lines of solar latitude in the south polar sector. For repetitive events with intervals between them being not so long, the dominant dimmings demonstrated a clear homology in their forms and locations. During the very powerful event of October 28, one homologous global set of dimmings changed to another set. Many dimmings were observed to be identical or very similar in the three coronal channels and the transition-region line. It follows from the analysis that rapidly recovering global structures in the corona and transition region were involved in the eruption of running CMEs and the corresponding reconstruction of the large-scale magnetic fields.