EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION
EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION
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基于 SDO/HMI 观测的主要喷发活跃区磁场和能量的演化
DOI：
10.1088/0004-637x/748/2/77
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发表时间：
2012
期刊：
影响因子：
--
通讯作者：
Thalmann
中科院分区：
文献类型：
--
作者：
Hoeksema;Wiegelmann;T.Hayashi;Thalmann
我们根据太阳动态观测站 (SDO) 上的日震和磁成像仪 (HMI) 的矢量磁图系列，报告了 NOAA 活动区域 11158 在五天内的磁场及其能量的演变。快速的通量出现和强烈的剪切运动导致了四极太阳黑子复合体，产生了几次重大喷发，包括太阳周期 24 的第一次 X 级耀斑。外推的非线性无力日冕场显示，在靠近低洼乙形细丝的早期通量出现期间，电流和自由能显着增加，细丝通道中具有剪切千高斯场。计算出的磁自由能最大值达到～2.6×10 32 erg，其中约50%存储在6 Mm以下。在 X 级耀斑发生后 1 小时内，它减少～ 0.3× 10 32 erg，这可能低估了实际能量损失。耀斑期间，光球场发生快速变化：核心区域水平场增强了28%，变得更加倾斜并且更加平行于极性反转线。这种变化与推测的日冕场“内爆”一致，并得到大气成像组件（AIA）观测到的日冕环回缩的支持。耀斑后外推场变得更加“紧凑”，核心区域的环路更短，可能是由于重新连接。日冕场在最低层的剪切力稍强，随着高度的增加松弛得更快，并且总体上能量较低。
We report the evolution of the magnetic field and its energy in NOAA active region 11158 over five days based on a vector magnetogram series from the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamic Observatory (SDO). Fast flux emergence and strong shearing motion led to a quadrupolar sunspot complex that produced several major eruptions, including the first X-class flare of Solar Cycle 24. Extrapolated nonlinear force-free coronal fields show substantial electric current and free energy increase during early flux emergence near a low-lying sigmoidal filament with a sheared kilogauss field in the filament channel. The computed magnetic free energy reaches a maximum of∼ 2.6× 10 32 erg, about 50% of which is stored below 6 Mm. It decreases by∼ 0.3× 10 32 erg within 1 hr of the X-class flare, which is likely an underestimation of the actual energy loss. During the flare, the photospheric field changed rapidly: the horizontal field was enhanced by 28% in the core region, becoming more inclined and more parallel to the polarity inversion line. Such change is consistent with the conjectured coronal field" implosion" and is supported by the coronal loop retraction observed by the Atmospheric Imaging Assembly (AIA). The extrapolated field becomes more" compact" after the flare, with shorter loops in the core region, probably because of reconnection. The coronal field becomes slightly more sheared in the lowest layer, relaxes faster with height, and is overall less energetic.
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