自適應(yīng)光學(xué)系統(tǒng)的多激光導(dǎo)星波前重構(gòu)算法研究
發(fā)布時間：2018-08-09 19:52
【摘要】：通常自適應(yīng)光學(xué)系統(tǒng)是將被成像目標(biāo)的光能量分出60%以上用于波前探測。此外自適應(yīng)光學(xué)系統(tǒng)通常所使用的哈特曼波前探測器,是用子孔徑將望遠鏡接收波前分割為直徑只有10cm左右的子波前,通過一一探測子光束的波前傾斜來重構(gòu)望遠鏡接收的整體波前,此處限定了子孔徑接收的光能量只相當(dāng)10cm口徑的望遠鏡,因此傳統(tǒng)的自適應(yīng)光學(xué)系統(tǒng)能夠校正成像的極限星等只有5星等!利用激光導(dǎo)星來探測波前,不僅能提高成像目標(biāo)的極限星等,而且使自適應(yīng)光學(xué)系統(tǒng)能對分布在大視場中的多目標(biāo)同時成像。但是,激光導(dǎo)星能發(fā)射的高度相對被成像目標(biāo)來說低得多,導(dǎo)致探測的波前缺失信息產(chǎn)生非等暈誤差。因此采用多個導(dǎo)星彌補波前信息缺失、進行波前的信息融合與重構(gòu)是導(dǎo)星探測技術(shù)的關(guān)鍵。本論文首先按照普遍認可的Hufnagel-Valley的大氣折射率結(jié)構(gòu)模型,以大氣折射率垂直分布函數(shù)為光通道分層權(quán)重分配依據(jù),采用高度各階原點矩算法計算各層等效面的高度位置,得出:大氣湍流對光波前有影響的通道為從地面到15km高度處,集中了全部大氣湍流的99.3%,也可以近似認為從地面到8km高度處,其中集中了全部大氣湍流的96%,;可將15km大氣通道分為近似等密度的三層或?qū)?km大氣通道分為近似等密度的二層:第一層從地面到1.65km,等效面高度為0.15km,湍流強度權(quán)重為88.2%;第二層從1.65km到8.00km,等效面高度為3.78km,湍流強度權(quán)重為7.1%;第三層從8.00km到15km,等效面高度為11.20km,湍流強度權(quán)重為4.0%。提出一種符合大氣湍流的空間統(tǒng)計特性和時間統(tǒng)計特性的動態(tài)相位屏生成方法,基于該方法建立了大氣湍流仿真程序,為波前重構(gòu)算法的驗證和分析提供了基礎(chǔ)。提出在地基望遠鏡的接收平面上多顆瑞利導(dǎo)星波前信號的平面加權(quán)波前重構(gòu)方法�；谙辔唤Y(jié)構(gòu)函數(shù),分別以每顆導(dǎo)星在地面的投影位置為中心,計算該導(dǎo)星的波前探測信號在望遠鏡接收口徑的徑向與方位上的權(quán)重分配函數(shù),進行多顆導(dǎo)星波面的加權(quán)融合,完成成像目標(biāo)的波前重構(gòu)。針對望遠鏡口徑為1.25m,大氣相干長度為10cm,采用5顆呈十字形排布、外接圓與望遠鏡口徑重合、高度為10km的瑞利導(dǎo)星,用平面加權(quán)算法模擬校正軸上目標(biāo)成像時,不考慮校正誤差的斯特列爾比理論上能夠達到0.49。進一步考慮10km高度以上大氣層的未采樣誤差,計算得到上層未采樣誤差為0.57rad,這樣波前探測的總誤差rms值增至1.02rad,換算為系統(tǒng)的斯特列爾比仍然可以達到0.35,說明五顆10km高度的瑞利導(dǎo)星能夠滿足實用要求。搭建了光學(xué)平臺上的檢驗光學(xué)系統(tǒng),實驗結(jié)果與理論值吻合,證明平面加權(quán)波前重構(gòu)的算法精度足夠高。對于4米以上大口徑望遠鏡的多層共軛自適應(yīng)光學(xué)成像的應(yīng)用,須使用發(fā)射高度90km的鈉導(dǎo)星,采用廣義tikhonov正則化的zernike模式分層解析重構(gòu)波前算法,避免投影矩陣條件數(shù)過大的問題。當(dāng)望遠鏡口徑為8m,大氣相干長度為12cm,采用3顆90km高度的鈉激光導(dǎo)星時,廣義tikhonov正則化的zernike模式分層解析波前重構(gòu)算法在1角分視場內(nèi)的平均誤差為0.68rad,其相應(yīng)的斯特列爾比達到0.63,為1.26倍衍射極限分辨能力。多層共軛自適應(yīng)光學(xué)系統(tǒng)中,鈉導(dǎo)星數(shù)量在3-5顆為宜,校正器數(shù)量在2-3個為宜,進一步增加導(dǎo)星數(shù)量和校正器的數(shù)量對自適應(yīng)系統(tǒng)性能的提高有限。導(dǎo)星的最佳分布為:2顆導(dǎo)星為直線分布,導(dǎo)星對應(yīng)視場中心張角為15.7″、三顆導(dǎo)星為正三角形分布,導(dǎo)星對應(yīng)視場中心張角為21.5″、四顆導(dǎo)星為正方形分布,導(dǎo)星對應(yīng)視場中心張角為23.5″、五顆導(dǎo)星為正五邊形分布,導(dǎo)星對應(yīng)視場中心張角為27.4″。最佳的校正器共軛高度只與大氣湍流強度的垂直分布有關(guān),使用兩個校正器時,其最佳共軛高度為0km和10km;使用三個校正器時,其最佳共軛高度為0km、2km和11km。本文提出的波前重構(gòu)算法以及得到的以上結(jié)論是對多激光導(dǎo)星自適應(yīng)光學(xué)系統(tǒng)實用化有益的探索研究,可將地面層自適應(yīng)光學(xué)模式的視場平均斯特列爾比從0.17提高到0.26,視場中心的的斯特列爾比從0.18提高到0.45。將對我國多激光導(dǎo)星自適應(yīng)光學(xué)系統(tǒng)的發(fā)展起到一定的推動作用。
[Abstract]:The adaptive optical system usually divides the light energy of the target to more than 60% for the wavefront detection. In addition, the Hartmann wavefront detector usually used in the adaptive optical system is to reconstruct the telescope before the wavefront of the telescope is divided into a wavelet with a diameter of only 10cm, and to reconstruct the wavefront of the sub beam to reconstruct the wavefront. The telescope received the whole wave front, where the optical energy received by the sub aperture is only equivalent to the 10cm aperture telescope, so the traditional adaptive optical system can correct the limit of imaging only 5 stars! Using the laser guide to detect the wavefront can not only improve the limit stars of the imaging target, but also make the adaptive optical system possible. However, the height of the laser guided star is much lower than that of the image target, which leads to the unequal halo error of the wavefront missing information of the detection. Therefore, it is the key to use multiple guides to make up for the missing wavefront information and the information fusion and reconstruction of the wavefront. Firstly, according to the universally recognized atmospheric refractive index structure model of Hufnagel-Valley, the vertical distribution function of atmospheric refractive index is used as the basis of the layered weight distribution of the optical channel, and the height of the equivalent surface of each layer is calculated by the height order moment algorithm. It is concluded that the channel of atmospheric turbulence affecting the wavefront is from the ground to the 15km height. 99.3% of all atmospheric turbulence can be concentrated, which can be approximately considered from the ground to 8km height, which concentrates 96% of the total atmospheric turbulence, and the 15km atmospheric channel can be divided into three layers of approximately equal density or the 8km atmosphere channel is divided into two layers of approximately equal density: the first layer is from the ground to the 1.65km, the equivalent surface height is 0.15km, and the turbulence intensity weight is weighted. For 88.2%, the second layer from 1.65km to 8.00km, the equivalent surface height is 3.78km, the weight of the turbulence intensity is 7.1%, the third layer from 8.00km to 15km, the equivalent surface height is 11.20km, and the weight of the turbulence intensity is 4.0%. to propose a dynamic phase screen generation method which conforms to the spatial statistical characteristics and the time statistical properties of atmospheric turbulence, and the atmosphere is based on this method. The turbulence simulation program provides a basis for the verification and analysis of the wavefront reconstruction algorithm. The plane weighted wavefront reconstruction method of multiple Rayleigh guide star wavefront signals on the receiving plane of the foundation telescope is proposed. Based on the phase structure function, the wavefront detection signal of the guide star is calculated at the center of the projection position of each guide star on the ground. The weighted fusion function of the radially and azimuth of the telescope receives the weighted fusion function of the telescope and carries out the weighted fusion of multiple star wavefronts to complete the wavefront reconstruction of the imaging target. For the telescope aperture is 1.25m, the atmospheric coherence length is 10cm, 5 zigzag arrangement, the overlap of the circle and the telescope aperture, the height of the Rayleigh guide with a height of 10km, is added to the plane. The weight algorithm simulates the correction of the target imaging on the axis, and does not consider the correction error in the steerr's theory, which can theoretically reach 0.49. to further consider the non sampling error of the atmosphere above the 10km height, and the upper layer error is calculated to be 0.57rad, so the total error RMS of the wavefront detection is increased to 1.02rad, converted to the system's steerratio. It can reach 0.35, indicating that the five 10km height Rayleigh guide can meet the practical requirements. The test optical system on the optical platform is built. The experimental results coincide with the theoretical value. It is proved that the algorithm of plane weighted wavefront reconstruction is accurate enough. For the application of multi-layer conjugate adaptive optical imaging for large aperture telescope over 4 meters, the application of the multi-layer conjugate adaptive optical imaging is necessary. Using a sodium guide star with a height of 90km, a generalized Tikhonov regularized Zernike mode layered analytic reconstruction wave front algorithm is used to avoid the problem of oversize of the projection matrix. When the telescope aperture is 8m, the atmospheric coherence length is 12cm, 3 90km height sodium laser guides are adopted, and the generalized Tikhonov regularization method of Zernike mode is analyzed. The average error of the wavefront reconstruction algorithm in the 1 angle field of view is 0.68rad, and its corresponding stellar ratio is 0.63 and the diffraction limit resolution is 1.26 times. In the multi-layer conjugate adaptive optical system, the number of sodium guide stars is 3-5, the number of corrector is 2-3, and the number of guide stars and the number of corrector are further increased to the adaptive system. The best distribution of the system is that the best distribution of the guide star is as follows: 2 guide stars are linear distribution, the guide star corresponding to the center of view is 15.7 ", the three guide stars are triangle distribution, the guide star corresponding to the center angle of the field of view is 21.5", the four guide star is square, the guide star corresponding to the center of view is 23.5 ", and the five star is the regular pentagon distribution. The center angle of the guide star is 27.4 ". The best conjugate height of the corrector is only related to the vertical distribution of the atmospheric turbulence intensity. When the two corrector is used, the best conjugate height is 0km and 10km. When using three corrector, the best conjugate height is the wavefront reconstruction algorithm and the above conclusion proposed in this paper, 0km, 2km and 11km.. The theory is a useful exploration for the practical application of the multi laser guide star adaptive optical system, which can increase the field of view of the adaptive optical mode of the ground layer from 0.17 to 0.26, and the STL ratio from 0.18 to 0.45. in the center of the field of view will give a certain push to the development of the self adaptive optical system of our country's multi laser guide star. Use.
【學(xué)位授予單位】：中國科學(xué)院研究生院(長春光學(xué)精密機械與物理研究所)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2016
【分類號】：O439
本文編號：2175138
[Abstract]:The adaptive optical system usually divides the light energy of the target to more than 60% for the wavefront detection. In addition, the Hartmann wavefront detector usually used in the adaptive optical system is to reconstruct the telescope before the wavefront of the telescope is divided into a wavelet with a diameter of only 10cm, and to reconstruct the wavefront of the sub beam to reconstruct the wavefront. The telescope received the whole wave front, where the optical energy received by the sub aperture is only equivalent to the 10cm aperture telescope, so the traditional adaptive optical system can correct the limit of imaging only 5 stars! Using the laser guide to detect the wavefront can not only improve the limit stars of the imaging target, but also make the adaptive optical system possible. However, the height of the laser guided star is much lower than that of the image target, which leads to the unequal halo error of the wavefront missing information of the detection. Therefore, it is the key to use multiple guides to make up for the missing wavefront information and the information fusion and reconstruction of the wavefront. Firstly, according to the universally recognized atmospheric refractive index structure model of Hufnagel-Valley, the vertical distribution function of atmospheric refractive index is used as the basis of the layered weight distribution of the optical channel, and the height of the equivalent surface of each layer is calculated by the height order moment algorithm. It is concluded that the channel of atmospheric turbulence affecting the wavefront is from the ground to the 15km height. 99.3% of all atmospheric turbulence can be concentrated, which can be approximately considered from the ground to 8km height, which concentrates 96% of the total atmospheric turbulence, and the 15km atmospheric channel can be divided into three layers of approximately equal density or the 8km atmosphere channel is divided into two layers of approximately equal density: the first layer is from the ground to the 1.65km, the equivalent surface height is 0.15km, and the turbulence intensity weight is weighted. For 88.2%, the second layer from 1.65km to 8.00km, the equivalent surface height is 3.78km, the weight of the turbulence intensity is 7.1%, the third layer from 8.00km to 15km, the equivalent surface height is 11.20km, and the weight of the turbulence intensity is 4.0%. to propose a dynamic phase screen generation method which conforms to the spatial statistical characteristics and the time statistical properties of atmospheric turbulence, and the atmosphere is based on this method. The turbulence simulation program provides a basis for the verification and analysis of the wavefront reconstruction algorithm. The plane weighted wavefront reconstruction method of multiple Rayleigh guide star wavefront signals on the receiving plane of the foundation telescope is proposed. Based on the phase structure function, the wavefront detection signal of the guide star is calculated at the center of the projection position of each guide star on the ground. The weighted fusion function of the radially and azimuth of the telescope receives the weighted fusion function of the telescope and carries out the weighted fusion of multiple star wavefronts to complete the wavefront reconstruction of the imaging target. For the telescope aperture is 1.25m, the atmospheric coherence length is 10cm, 5 zigzag arrangement, the overlap of the circle and the telescope aperture, the height of the Rayleigh guide with a height of 10km, is added to the plane. The weight algorithm simulates the correction of the target imaging on the axis, and does not consider the correction error in the steerr's theory, which can theoretically reach 0.49. to further consider the non sampling error of the atmosphere above the 10km height, and the upper layer error is calculated to be 0.57rad, so the total error RMS of the wavefront detection is increased to 1.02rad, converted to the system's steerratio. It can reach 0.35, indicating that the five 10km height Rayleigh guide can meet the practical requirements. The test optical system on the optical platform is built. The experimental results coincide with the theoretical value. It is proved that the algorithm of plane weighted wavefront reconstruction is accurate enough. For the application of multi-layer conjugate adaptive optical imaging for large aperture telescope over 4 meters, the application of the multi-layer conjugate adaptive optical imaging is necessary. Using a sodium guide star with a height of 90km, a generalized Tikhonov regularized Zernike mode layered analytic reconstruction wave front algorithm is used to avoid the problem of oversize of the projection matrix. When the telescope aperture is 8m, the atmospheric coherence length is 12cm, 3 90km height sodium laser guides are adopted, and the generalized Tikhonov regularization method of Zernike mode is analyzed. The average error of the wavefront reconstruction algorithm in the 1 angle field of view is 0.68rad, and its corresponding stellar ratio is 0.63 and the diffraction limit resolution is 1.26 times. In the multi-layer conjugate adaptive optical system, the number of sodium guide stars is 3-5, the number of corrector is 2-3, and the number of guide stars and the number of corrector are further increased to the adaptive system. The best distribution of the system is that the best distribution of the guide star is as follows: 2 guide stars are linear distribution, the guide star corresponding to the center of view is 15.7 ", the three guide stars are triangle distribution, the guide star corresponding to the center angle of the field of view is 21.5", the four guide star is square, the guide star corresponding to the center of view is 23.5 ", and the five star is the regular pentagon distribution. The center angle of the guide star is 27.4 ". The best conjugate height of the corrector is only related to the vertical distribution of the atmospheric turbulence intensity. When the two corrector is used, the best conjugate height is 0km and 10km. When using three corrector, the best conjugate height is the wavefront reconstruction algorithm and the above conclusion proposed in this paper, 0km, 2km and 11km.. The theory is a useful exploration for the practical application of the multi laser guide star adaptive optical system, which can increase the field of view of the adaptive optical mode of the ground layer from 0.17 to 0.26, and the STL ratio from 0.18 to 0.45. in the center of the field of view will give a certain push to the development of the self adaptive optical system of our country's multi laser guide star. Use.
【學(xué)位授予單位】：中國科學(xué)院研究生院(長春光學(xué)精密機械與物理研究所)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2016
【分類號】：O439
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