The sun is a layered structure. Each layer has its own unique physics characteristics, and the different layer radiates different frequency electromagnetic wave. To obtain the three-dimension fine structure of the solar atmosphere, it is necessary to break through imaging technology in multiple wavelength-bands high-resolution. Based on the sun's atmosphere high-resolution three-dimension images, combined with measurements of solar matter flow rate and magnetic field, the three-dimension dynamic model of the solar magnetic field can be created to support space weather forecasting related to sun activity.

The research on solar adaptive optics technology is started in 1998. Under the key program of “Application of Adaptive Optics in High-resolution Observation of Sun”, CAE Member JIANG Wenhan and research professor RAO Changhui initiated and leaded a solar adaptive team. The team developed the first tip/tilt-corrected adaptive optical system for 43cm solar telescope of Nanjing University to improved tracking precision of sun image and decrease images jitter in China. In addition, with the support of Yunnan Observatory, the team built an adaptive optical system for 26cm solar telescope of Yunnan Observatory and conducted a series high-resolution imaging experiments and achieved high–resolution images of sunspot and sun’s granulation structure in at home in 2009. Furthermore, the team was awarded the funding from Astronomy Joint fund of national natural science foundation of China on “high –resolution adaptive optical imaging technologies the one meter infrared solar tower of Yunnan Observatory in mid July 2011”.

The observation results of sunspot and sun’s granulation structure are shown in Fig.1 and Fig 2.

　　　　　　　　　  (a)　Results without AO　　　　　　 (b)　Results with AO

　　Fig.1: Image of sunspot achieved in visible (wavelength: 7100Å) (Image by solar adaptive team)

　　　　　　　　　   (a)　Results without AO　　　　　　 (b)　Results with AO

Fig.2: Image of sunspot achieved in NIR (wavelength:15550Å) (Image by solar adaptive team)