太阳耀斑期间光球磁场结构的突然运动意味着发生在日冕中的剧烈能量释放过程可能足以扰动光球层。本项目拟了解有多大比例的耀斑会产生光球的扰动，以及是不是所有能级的耀斑都会产生光球扰动。本项目拟分析光球扰动伴随的磁场螺度输运模式、被扰动的光球磁场结构对应的光球磁场变化和光球洛伦兹力的变化、对应的日冕磁场结构的变化，从而探讨耀斑扰动光球层的物理机制。. 本项目主要采用NASA/SDO卫星的HMI光球矢量场数据以及云南天文台NVST的矢量场数据和高时空分辨率的光球像数据。其中SDO提供了大量的耀斑事件的矢量场数据；NVST的高分辨数据有利于探测耀斑期间光球特征的更细微的水平运动。

The abrupt motions of the magnetic structures on the photosphere during a solar flare could be a result of the energy release in the solar corona. Here, we will survey what percentage of the flares can produce obvious motions of the photospheric structures and whether the motions on the photosphere can occur in flares with various energy ranges. To study how the energy release in the corona produces the abrupt photospheric motions, we will investigate the changes in the transportations of the magnetic helicity across the photosphere accompanying with the abrupt photospheric motions, the changes in the Lorentz force acted on the photospheric structures, and the changes in the coronal magnetic systems connecting the photospheric structures disturbed by the flares.. The data used here mainly includes the first uninterrupted time series of space-based, full-disk, vector magnetic field observations of the Sun with a at least 12-minute cadence from SDO/HMI, as well as the vector magnetic data and the photospheric images with high-resolution from NVST. The HMI data enables us to detect the motions of the photospheric structures during a host of flares, while NVST data allows a detailed examination of the smaller displacement of the structures on the photosphere during the flare.