Hinode Observations of a Vector Magnetic Field Change Associated with a Flare on 2006 December 13
Hinode Observations of a Vector Magnetic Field Change Associated with a Flare on 2006 December 13
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DOI：
10.1093/pasj/59.sp3.s779
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发表时间：
2007-09
影响因子：
2.3
通讯作者：
M. Kubo;T. Yokoyama;Y. Katsukawa;B. Lites;S. Tsuneta;Y. Suematsu;K. Ichimoto;T. Shimizu;S. Nagata;T. Tarbell;R. Shine;A. Title;D. Elmore
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文献类型：
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作者：
M. Kubo;T. Yokoyama;Y. Katsukawa;B. Lites;S. Tsuneta;Y. Suematsu;K. Ichimoto;T. Shimizu;S. Nagata;T. Tarbell;R. Shine;A. Title;D. Elmore
2006年12月6日至19日期间，利用日出号航天器上的太阳光学望远镜成功地对耀斑活动区10930进行了连续观测。我们专注于光球磁场在这个活动区域的演变，并在现场的X3.4级耀斑的磁场特性，使用一个时间序列的矢量场地图与高空间分辨率。X3.4级耀斑发生在2006年12月13日，在巨大的相反极性的本影之间的明显碰撞地点。在耀斑爆发前一天，在碰撞地点的半影区出现了由磁通量出现引起的正负极性交替的细长磁结构。随后，在碰撞现场的极性反转线变得非常复杂。在这些细长的磁性结构的形成过程中，在Ca II H的明亮的环路的数量增加。耀斑带和亮环沿着极性反转线演化，亮环的一个足点位于磁场方位角相对于周围环境偏离较大的区域。高空间分辨率和高偏振精度的SOT观测揭示了耀斑现场磁场精细结构的时间变化：复杂的极性反转线的某些部分消失了，在这些区域，光球磁场的方位角改变了约90 i，在碰撞现场内变得更加空间均匀。
Continuous observations of the flare productive active region 10930 were successfully carried out with the Solar Optical Telescope aboard the Hinode spacecraft during 2006 December 6 to 19. We focused on the evolution of photospheric magnetic fields in this active region, and the magnetic field properties at the site of the X3.4 class flare, using a time series of vector field maps with high spatial resolution. The X3.4 class flare occurred on 2006 December 13 at the apparent collision site between the large, opposite polarity umbrae. Elongated magnetic structures with alternatingly positive and negative polarities resulting from flux emergence appeared one day before the flare in the collision site penumbra. Subsequently, the polarity inversion line at the collision site became very complicated. The number of bright loops in Ca II H increased during the formation of these elongated magnetic structures. Flare ribbons and bright loops evolved along the polarity inversion line and one footpoint of the bright loop was located in a region having a large departure of the field azimuth angle with respect to its surroundings. SOT observations with high spatial resolution and high polarization precision revealed temporal change in the fine structure of magnetic fields at the flare site: some parts of the complicated polarity inversion line then disappeared, and in those regions the azimuth angle of the photospheric magnetic field changed by about 90i, becoming more spatially uniform within the collision site.