【摘要】：撫仙湖1 m新真空太陽望遠(yuǎn)鏡(New Vacuum Solar Telescope,NVST)作為目前國(guó)內(nèi)口徑最大的地基太陽望遠(yuǎn)鏡,有著給太陽物理研究人員提供高質(zhì)量高分辨率的觀測(cè)數(shù)據(jù)的使命。統(tǒng)計(jì)傳遞函數(shù)的正確估計(jì)是NVST圖像重建的關(guān)鍵一步,但是望遠(yuǎn)鏡像差、光子噪聲、非等暈效應(yīng)等因素都可能使傳遞函數(shù)的估計(jì)產(chǎn)生偏差。在高分辨太陽數(shù)據(jù)的實(shí)際數(shù)據(jù)處理中,統(tǒng)計(jì)傳遞函數(shù)的估計(jì)誤差會(huì)導(dǎo)致高分辨數(shù)據(jù)處理結(jié)果分辨率降低,甚至失真。所以必須要研究統(tǒng)計(jì)傳遞函數(shù)的估計(jì)誤差對(duì)高分辨圖像重建結(jié)果的影響,從而獲得更好分辨率的重建圖像。本文基于斑點(diǎn)重構(gòu)算法理論,采用理論推導(dǎo)、數(shù)值模擬、實(shí)測(cè)數(shù)據(jù)重建三者結(jié)合的方式研究了像差、噪聲、非等暈效應(yīng)對(duì)NVST高分辨算法重建結(jié)果的影響,主要考慮兩個(gè)方面:1.誤差對(duì)算法重建目標(biāo)傅里葉模的影響;2.誤差對(duì)算法重建目標(biāo)相位的影響。本文完成的主要工作如下:1)分析了相同大氣視寧度情況下,同類型像差不同像差大小對(duì)NVST高分辨重建結(jié)果的影響;相同大氣視寧度情況下,不同類型像差相同像差大小對(duì)NVST高分辨重建結(jié)果的影響;視寧度不同時(shí),同類型像差相同像差大小對(duì)NVST高分辨重建結(jié)果的影響。2)分析了光子噪聲對(duì)圖像功率譜重建的影響;不同大氣視寧度常數(shù)情況下,不同光子噪聲對(duì)譜比曲線的影響;不同大氣視寧度常數(shù),不同光子噪聲對(duì)NVST算法重建結(jié)果的影響以。3)推導(dǎo)了非等暈效應(yīng)對(duì)斑點(diǎn)干涉術(shù)、斑點(diǎn)掩模法、譜比法估計(jì)傳遞函數(shù)的影響。采用數(shù)值模擬的方法模擬出了非等暈效應(yīng),以不同子塊大小對(duì)實(shí)測(cè)光球數(shù)據(jù)進(jìn)行重建,使用圖像平均功率譜分析了非等暈效應(yīng)對(duì)NVST高分辨圖像重建結(jié)果的影響。當(dāng)像差大小不超過一定范圍時(shí),像差并不會(huì)對(duì)重建結(jié)果產(chǎn)生太大影響。當(dāng)像差大小超過一定范圍時(shí),像差會(huì)影響重建結(jié)果且隨著像差的增加和大氣視寧度的變好這種影響會(huì)更加明顯。離焦像差和球差對(duì)圖像重建影響比較大。光子噪聲在斑點(diǎn)圖功率譜引入了偏差,在重建的時(shí)候會(huì)出現(xiàn)一種高頻放大現(xiàn)象,導(dǎo)致研究人員想要重建的高頻信息無法有效復(fù)原。在大氣視寧度相對(duì)比較好的時(shí)候,光子噪聲對(duì)譜比曲線的影響比較大,這會(huì)使對(duì)斑點(diǎn)干涉術(shù)傳遞函數(shù)的估計(jì)有偏差。在視寧度相對(duì)比較差的時(shí)候,光子噪聲會(huì)使重譜法遞推相位的重建精度明顯降低。非等暈誤差對(duì)大視場(chǎng)目標(biāo)重建存在影響,會(huì)使斑點(diǎn)干涉術(shù)重建結(jié)果不準(zhǔn)確而導(dǎo)致圖像分辨率下降。為了重建圖像有更好的分辨率,最好以等暈區(qū)大小分塊,這樣非等暈效應(yīng)的影響最小,甚至可以忽略。
[Abstract]:As the largest ground-based solar telescope in China, Fuxian Lake 1 m vacuum Solar Telescope (New Vacuum Solar Telescope,NVST) has the mission of providing high quality and high resolution observation data to Heliophysical researchers. The correct estimation of the statistical transfer function is a key step in the reconstruction of NVST images, but the aberration of the telescope, the photon noise and the non-isobaric effect may lead to the deviation of the estimation of the transfer function. In the actual data processing of high-resolution solar data, the estimation error of the statistical transfer function will result in the resolution of the high-resolution data processing reduced or even distorted. Therefore, it is necessary to study the effect of the estimation error of statistical transfer function on the reconstruction results of high-resolution images, so as to obtain a better resolution of reconstructed images. Based on the theory of speckle reconstruction algorithm, the effects of aberration, noise and non-equal-halo effect on the reconstruction results of NVST high resolution algorithm are studied by theoretical derivation, numerical simulation and real data reconstruction. Two main considerations: 1. The effect of error on the Fourier mode of target reconstruction. 2. The effect of error on the phase reconstruction of target. The main work of this paper is as follows: 1) the effects of different aberrations of the same type of aberrations on the reconstruction results of NVST with the same atmospheric apparent degree are analyzed. The effect of the same aberration size of different types of aberrations on the high resolution reconstruction results of NVST under the same atmospheric apparent intensity; The effect of the same type aberration and the same aberration on the reconstruction results of NVST high resolution is analyzed. 2) the influence of photon noise on image power spectrum reconstruction is analyzed. The influence of different photon noise on the spectral ratio curve under different atmospheric apparent degree constants; Effects of different Atmospheric apparent Nine constants and different Photon noise on the Reconstruction results of NVST algorithm. 3) the effects of non-equal-halo effect on speckle interferometry speckle mask method and spectral ratio method for estimating transfer function are derived. The non-equal-halo effect is simulated by numerical simulation, and the measured optical sphere data are reconstructed with different sub-block sizes. The effect of non-equal-halo effect on the reconstruction results of NVST high-resolution image is analyzed by using the average power spectrum of the image. When the aberration is not larger than a certain range, the aberration does not have much influence on the reconstruction results. When the aberration is larger than a certain range, the aberration will affect the reconstruction result and become more obvious with the increase of aberration and the improvement of atmospheric apparent degree. Defocus aberration and spherical aberration have great influence on image reconstruction. Photon noise induces bias in speckle power spectrum, and a high frequency amplification phenomenon occurs during reconstruction, which leads to the failure to recover the high frequency information that researchers want to reconstruct. When the atmospheric apparent degree is relatively good, the photon noise has a great influence on the spectral ratio curve, which will make the estimation of the speckle interferometry transfer function biased. When the apparent noise is relatively poor, the reconstruction accuracy of the recursive phase of the respectral method is obviously reduced by the photon noise. The effect of non-equal-halo error on the reconstruction of large field of view object will make the reconstruction result of speckle interferometry inaccurate and result in the decrease of image resolution. In order to improve the resolution of the reconstructed image, it is better to divide the image into blocks with the size of the equal-halo region, so that the effect of the non-isobaric effect can be minimized or even ignored.
【學(xué)位授予單位】：中國(guó)科學(xué)院大學(xué)(中國(guó)科學(xué)院云南天文臺(tái))
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2017
【分類號(hào)】：P111.41

【參考文獻(xiàn)】

相關(guān)期刊論文 前10條

1 豐帆;李常偉;;基于小波分析的大氣湍流相位屏模擬[J];光學(xué)學(xué)報(bào);2017年01期

2 向永源;劉忠;金振宇;楊磊;;高分辨率太陽圖像重建方法[J];天文學(xué)進(jìn)展;2016年01期

3 方玉亮;金振宇;劉忠;戴懿純;黃善杰;;一米新真空太陽望遠(yuǎn)鏡離焦對(duì)高分辨太陽觀測(cè)圖像重建的影響[J];天文研究與技術(shù);2015年02期

4 鐘立波;田雨;饒長(zhǎng)輝;;靜態(tài)像差對(duì)交叉譜相位復(fù)原精度的影響及補(bǔ)償方法[J];光學(xué)學(xué)報(bào);2014年07期

5 Zhong Liu;Jun Xu;Bo-Zhong Gu;Sen Wang;Jian-Qi You;Long-Xiang Shen;Ru-Wei Lu;Zhen-Yu Jin;Lin-Fei Chen;Ke Lou;Zhi Li;Guang-Qian Liu;Zhi Xu;Chang-Hui Rao;Qi-Qian Hu;Ru-Feng Li;Hao-Wen Fu;Feng Wang;Men-Xian Bao;Ming-Chan Wu;Bo-Rong Zhang;;New vacuum solar telescope and observations with high resolution[J];Research in Astronomy and Astrophysics;2014年06期

6 劉艷霄;楊云飛;林雋;;太陽光球磁亮點(diǎn)的識(shí)別算法[J];天文研究與技術(shù);2014年02期

7 汪景t;季海生;;空間天氣驅(qū)動(dòng)源——太陽風(fēng)暴研究[J];中國(guó)科學(xué):地球科學(xué);2013年06期

8 劉忠;鄧元勇;季海生;黎輝;;中國(guó)地基大太陽望遠(yuǎn)鏡[J];中國(guó)科學(xué):物理學(xué) 力學(xué) 天文學(xué);2012年12期

9 ;Recent progress of solar physics research in China[J];Research in Astronomy and Astrophysics;2011年12期

10 向永源;金振宇;;斑點(diǎn)干涉術(shù)統(tǒng)計(jì)結(jié)果的信噪比模擬和分析[J];天文研究與技術(shù);2011年03期

相關(guān)博士學(xué)位論文 前5條

1 向永源;太陽高分辨高速重建算法的研究[D];中國(guó)科學(xué)院研究生院(云南天文臺(tái));2016年

2 鐘立波;太陽高分辨力圖像重建技術(shù)研究[D];中國(guó)科學(xué)院研究生院（光電技術(shù)研究所）;2015年

3 史廣維;基于矢量波像差理論的反射望遠(yuǎn)系統(tǒng)裝調(diào)研究[D];中國(guó)科學(xué)院研究生院（長(zhǎng)春光學(xué)精密機(jī)械與物理研究所）;2011年

4 解妍瓊;太陽風(fēng)暴的綜合研究[D];中國(guó)科學(xué)院研究生院（空間科學(xué)與應(yīng)用研究中心）;2007年

5 劉忠;天文圖象高分辨重建及空域性質(zhì)研究[D];中國(guó)科學(xué)院研究生院（云南天文臺(tái)）;2003年

相關(guān)碩士學(xué)位論文 前1條

1 王思博;NVST成像系統(tǒng)觀測(cè)數(shù)據(jù)干涉條紋研究與處理[D];中國(guó)科學(xué)院研究生院(云南天文臺(tái));2016年

，

本文編號(hào)：2371073