太阳是一个巨大的磁等离子体，其间的一切现象和过程都受到太阳磁场的调控，同时，太阳磁场还通过冕洞区的开放的磁力线结构将其影响延伸到日地空间及整个日球区域，因此太阳磁场的研究对影响人类高科技环境的空间灾害性天气的预报和监测具有根本性的意义。本文通过对2004年8月8日至19日国际编号为AR10656的太阳活动区发生的太阳耀斑事件的分析去了解太阳活动的磁场演化和太阳活动与磁非势参量的联系，从而可以更好的进行太阳活动预报和监测。活动区AR10656发生了大量的耀斑事件，观测到的耀斑级别从微耀斑到大耀斑都有覆盖。本文主要分析了中国科学院国家天文台怀柔太阳观测基地和美国大熊湖天文台的观测资料，来研究矢量磁场的演化。首先分析磁场位形和非势特性的演化。然后使用Yan等[1]的边界元方法程序进行了磁场外推。磁流浮现和对消以及由此带来的磁非势特性变化与大耀斑活动有关。与其它一些太阳超级活动区相比，这一活动区的磁场位形和非势参量的变化更加缓慢，并且能量传输和释放过程也相对较慢。这一缓慢的过程可能是导致该活动区重现耀斑事件不断发生的原因。

The sun is a huge magnetic plasma. All the phenomenon and processes are under the effect of the magnetic field. And the solar magnetic field can extend to affect space between the sun and the earth, and the whole heliosphere by the open structure of magnetic line from solar coronal hole. Thus, the study of solar magnetic field is ultimately important for forecasting and monitoring the space weather, where the human high-tech projects are performed.A recurrent solar flare activity including micro to major flares was observed in NOAA Active Region 10656 between 08 and 19 August 2004. In this paper, we will study the evolution of vector magnetic field by using the observations of Huairou Solar Observing Station (HSOS, China) and Big Bear Solar Observatory (BBSO, USA). The evolution of magnetic morphology and non-potentiality are analyzed firstly. And then, the magnetic extrapolation is carried out based on the boundary element method developed by Yan et al. [1] The magnetic flux emergence and cancellation, and thus, magnetic non-potential changes, are associated with the major flares. Compared with some other super active regions, the evolution of magnetic morphologies and non-potentialities are more gradual, and thus the energy transportation and release are relatively slow. This gradual process may result in the recurrent flares.