Magnetic flux evolution inside and outside a polar coronal hole based on data from the Solar Dynamics Observatory (SDO)
Magnetic flux evolution inside and outside a polar coronal hole based on data from the Solar Dynamics Observatory (SDO)
复制标题
基于太阳动力学观测站 (SDO) 数据的极冕洞内外磁通量演化
DOI：
10.1134/s0016793212070031
复制
发表时间：
2012
影响因子：
0.6
通讯作者：
E. Benevolenskaya
中科院分区：
文献类型：
--
作者：
E. Benevolenskaya
本文介绍了2010年8月1-2日期间，对一个北方极冕洞内外磁场的分析结果。极冕洞的位置是由太阳动力学天文台（SDO）的大气成像仪组件（AIA）获得的Fe XII，XXIV（193）线的极紫外（EUV）图像确定的。磁数据由磁场强度的视线分量表示，用日震和磁成像仪（HMI）测量。两个数据集均以720秒的间隔进行采样，并重新映射到卡林顿坐标网格上，分辨率为正弦纬度0.001和经度0.1度。初步结果显示，新周期的极性（北极的正极性）的磁通量出现在日冕洞内，时间尺度为几个小时。这种“新通量”与旧太阳周期的磁通量（北方的负极性）无关。
This paper presents the analysis results of the magnetic flux inside and outside a polar coronal hole in the north during the period August 1–2, 2010. The location of the polar coronal hole is determined from Extreme Ultraviolet (EUV) images in the Fe XII, XXIV (193 Å) line, obtained by an Atmospheric Imager Assembly (AIA) of the Solar Dynamics Observatory (SDO). Magnetic data are represented by the line-of-sight component of the magnetic field strength, measured with an Helioseismic and Magnetic Imager (HMI). Both data sets are sampled at an interval of 720 s and are remapped onto a Carrington coordinate grid with a resolution of 0.001 in sine latitude and 0.1 degree in longitude. The preliminary results show a magnetic flux of the new cycle’s polarity (positive polarity in the north) appearing inside the coronal hole on a time scale of several hours. This “new flux” does not correlate with the magnetic flux of the old solar cycle (negative polarity in the north).