一系列同源局限耀斑的能量起源和触发机制
Energy origination and triggering mechanism of a series of homologous confined flares
摘要：
利用新真空太阳望远镜（NVST）的H $α$资料，结合太阳动力学观测站（SDO）的多波长图像和磁象图，研究了2013年10月12日NOAA 11861活动区发生的3次同源受限耀斑的详细过程。这三次耀斑都发生在同一位置，具有相似的形态和类似的类别。通过对磁场和流场演化的分析，发现在后黑子附近出现了磁通量和强的两极间剪切运动。磁通量和平均横向磁场强度在每次喷发前均呈下降趋势，并在每次喷发开始时达到最低点。通过计算光球层的剪切和出射能量，发现光球层注入的能量在几个小时内的积分可以为耀斑提供足够的能量。在每次耀斑发生期间，在H $α$图像中观察到不同环之间的重新连接。这些结果表明，光球层中的出射磁通量和剪切运动可以将能量注入剪切磁环，并最终通过磁重联释放能量，为太阳耀斑提供能量。
英文摘要：
Using the H$α$ data from the New Vacuum Solar Telescope (NVST) at the Fuxian Solar Observatory together with multi-wavelength images and magnetograms obtained by Solar Dynamics Observatory (SDO), we study the detailed process of three homologous confined flares in active-region (AR) NOAA 11861 on 2013 October 12. All of the three flares occurred at same location, with similar morphologies and comparable class. Through analyzing the evolution of magnetic field and flow field, we found an emergence of magnetic flux and a strong shearing motion between two opposite polarities near the following sunspot. The magnetic flux and the average transverse field strength exhibited a decrease before each eruption and reached the lowest point at the onset of each eruption. By calculating the shearing and the emergence energy in the photosphere, we found that the integral of energy injected from the photosphere, for a few hours, could provide enough energy for the flares. The reconnection between different loops was observed in H$α$ images during the occurrence of each flare. These results suggest that the emerging magnetic flux and the shearing motion in the photosphere can inject the energy to the sheared magnetic loops and the energy finally was released via magnetic reconnection to power the solar flares.
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