Solar image reconstruction method under atmospheric turbulence at Fuxian Lake Solar Observatory  

作　　者：Sizhong Zou Zhenyu Jin Kaifan Ji Jun Xu Lei Yang 

机构地区：[1]Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China [2]Yunnan Key Laboratory of Solar Physics and Space Science,Kunming 650216,China [3]University of Chinese Academy of Sciences,Beijing 101408,China

出　　处：《Astronomical Techniques and Instruments》2024年第2期128-139,共12页天文技术与仪器（英文）

基　　金：sponsored by the National Natural Science Foundation of China(NSFC)under the grant numbers(11773073,11873027,U2031140,11833010);Yunnan Key Laboratory of Solar Physics and Space Science under the number 202205AG070009;Yunnan Provincial Science and Technology Department(202103AD50013,202105AB160001,202305AH340002);the GHfund A202302013242 and CAS“Light of West China”Program 202305AS350029.

摘　　要：Strong atmospheric turbulence reduces astronomical seeing,causing speckle images acquired by ground-based solar telescopes to become blurred and distorted.Severe distortion in speckle images impedes image phase deviation in the speckle masking reconstruction method,leading to the appearance of spurious imaging artifacts.Relying only on linear image degradation principles to reconstruct solar images is insufficient.To solve this problem,we propose the multiframe blind deconvolution combined with non-rigid alignment(MFBD-CNRA)method for solar image reconstruction.We consider image distortion caused by atmospheric turbulence and use non-rigid alignment to correct pixel-level distortion,thereby achieving nonlinear constraints to complement image intensity changes.After creating the corrected speckle image,we use the linear method to solve the wavefront phase,obtaining the target image.We verify the effectiveness of our method results,compared with others,using solar observation data from the 1 m new vacuum solar telescope(NVST).This new method successfully reconstructs high-resolution images of solar observations with a Fried parameter r0 of approximately 10 cm,and enhances images at high frequency.When r0 is approximately 5 cm,the new method is even more effective.It reconstructs the edges of solar graining and sunspots,and is greatly enhanced at mid and high frequency compared with other methods.Comparisons confirm the effectiveness of this method,with respect to both nonlinear and linear constraints in solar image reconstruction.This provides a suitable solution for image reconstruction in ground-based solar observations under strong atmospheric turbulence.

关 键 词：Astronomical seeing Solar telescopes Solar observatories Astronomy image processing Phase error DECONVOLUTION 

分 类 号：P182[天文地球—天文学] P112