太阳爆发的能量积累机制研究

我们拟利用太阳动力学天文台（SDO）卫星上日震和磁场成像仪（HMI）高时空分辨率且在时间和空间上都完整的向量磁场观测数据，跟踪活动区从出现之前直到爆发事件发生的整个过程。研究磁流浮现活动区在浮现过程中能量的积累过程和机制，探讨磁流浮现和剪切运动在活动区能量积累中的作用，同时通过非线性无力场外推等方法结合SDO上大气成像仪器组（AIA）提供的日冕观测图像分析活动区上空能量密度的时间演化和空间分布特性，讨论能量积累及空间分布与太阳爆发活动之间的关系，进而讨论根据各种模型确定的能量积累的时间特性来预测爆发事件的发生的可能性。

We intend to use the full-disk vector magnetic field data with high temporal and spatial resolution and full time and space coverage from the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) satellite to track the full evolutionary process of active regions from before their appearance until the occurrence of eruptive phenomena. We plan to use the data to study the energy accumulation processes and mechanisms during emergence of active regions, to investigate the relative contribution of flux emergence and shear motion to the energy accumulation. Meanwhile, we will employ the non-linear force free field (NLFFF) method and compare the reconstructed coronal structures with the Atmospheric Imager Assembly (AIA) on SDO to study the temporal evolution and spatial distribution of magnetic energy density in the corona above active regions, and explore the relationship between energy accumulation and distribution and solar eruptions. We will also discuss the possibility to predict solar activities based on the temporal nature of the magnetic energy accumulation.