本文選題：拉曼阿爾法 + 光學(xué)設(shè)計(jì)��； 參考：《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)》2014年博士論文

【摘要】：日冕是太陽(yáng)大氣的最外層，從過(guò)渡區(qū)頂部向外延伸到幾個(gè)太陽(yáng)半徑，甚至更遠(yuǎn)的區(qū)域。日冕活動(dòng)對(duì)地球周?chē)臻g環(huán)境變化影響重大，是空間天氣預(yù)報(bào)的關(guān)鍵部分之一，，對(duì)日冕的觀測(cè)研究對(duì)太陽(yáng)物理學(xué)、人類活動(dòng)乃至對(duì)國(guó)家經(jīng)濟(jì)生活和太陽(yáng)物理學(xué)研究具有重要意義。 Lyman-alpha(拉曼阿爾法)輻射在太陽(yáng)物理學(xué)和日冕物理學(xué)中占據(jù)了非常重要的地位，作為色球?qū)庸庾V的主要成分，可以通過(guò)拉曼阿爾法光譜的觀測(cè)分析出色球?qū)拥闹饕Y(jié)構(gòu)。對(duì)于日冕成像最大的困難是：日冕的亮度相對(duì)太陽(yáng)光球?qū)雍蜕驁?chǎng)而言極為微弱，因此日冕儀的設(shè)計(jì)需要重點(diǎn)考慮日面照射到儀器上所引起的入瞳邊緣衍射和主鏡面自身散射的問(wèn)題。 本文首先介紹了日冕儀的發(fā)展歷史和透射式日冕儀的基本原理，針對(duì)外遮光日冕儀的外部遮光器圓盤(pán)遮擋效果和邊緣衍射光線進(jìn)行了理論性計(jì)算。 針對(duì)日冕儀反射式結(jié)構(gòu)，提出了入瞳位置假設(shè)，并在軸上近似條件下計(jì)算了主物鏡，次鏡和成像反射鏡的位置，進(jìn)一步的計(jì)算和討論了全反射式日冕儀在軸上理想成像近似時(shí)，入瞳成像即里奧光闌的位置是場(chǎng)鏡和成像鏡的焦距與間距的函數(shù)；在相同的近似條件下，得到了里奧光闌的尺寸計(jì)算公式，是關(guān)于三個(gè)物鏡的焦距和間距的函數(shù)，這對(duì)以后的全反射日冕儀設(shè)計(jì)一定的參考價(jià)值。 設(shè)計(jì)了口徑為40mm、焦距為590mm的全反射式拉曼阿爾法日冕儀，傳遞函數(shù)接近衍射極限。利用光學(xué)分析軟件建模分析了雜光情況：像面上接收入瞳邊緣衍射能量約為入射能量的6.8×10-9，提出主鏡面的加工要求。 設(shè)計(jì)并裝調(diào)一套球面反射式日冕儀實(shí)驗(yàn)裝置，建立光學(xué)分析仿真模型，采用點(diǎn)源透射率PST曲線的方法測(cè)量了此日冕儀的雜散光水平，通過(guò)對(duì)比實(shí)際像面上子午面的雜光分布曲線，驗(yàn)證了仿真模型的有效性。 最后對(duì)比了計(jì)算和測(cè)量光學(xué)系統(tǒng)雜散光的方法，根據(jù)雜光系數(shù)和PST函數(shù)關(guān)系式計(jì)算得到反射式日冕儀實(shí)驗(yàn)裝置的雜光系數(shù)為0.278。
[Abstract]:The corona is the outermost part of the sun's atmosphere, extending from the top of the transition zone to several solar radii or beyond. Coronal activity has a great influence on the change of space environment around the earth and is one of the key parts of space weather forecast. Human activities and even the study of national economic life and solar physics are of great significance. Lyman-alpha-alpha radiation plays an important role in solar physics and coronal physics. As the main component of chromospheric spectrum, the main structure of chromosphere can be analyzed by the observation of Raman Alpha-alpha spectrum. The biggest difficulty with coronal imaging is that the brightness of the corona is extremely weak relative to the solar sphere layer and the color field. Therefore, the design of coronal instrument should focus on the problems of the diffraction of the entrance pupil edge and the scattering of the main mirror itself caused by the solar surface irradiating to the instrument. In this paper, the development history of coronal apparatus and the basic principle of transmission coronatometer are introduced, and the theoretical calculation of the external shading effect and the edge diffraction light of the external shading coronal apparatus is carried out. In view of the reflective structure of coronal instrument, the assumption of entrance pupil position is put forward, and the positions of primary objective, secondary mirror and imaging mirror are calculated under the condition of axial approximation. The ideal imaging approximation of full reflection coronal instrument on axis is further calculated and discussed. The location of the Leo aperture is a function of the focal length and the spacing of the field mirror and the imaging mirror. Under the same approximate conditions, the calculation formula of the size of the Leo aperture is obtained, which is a function of the focal length and the spacing of the three objective lenses. This will be of reference value to the design of the coronal instrument of total reflection in the future. A full reflection Raman alpha corona instrument with a aperture of 40 mm and focal length of 590mm is designed. The transfer function is close to the diffraction limit. The optical analysis software is used to model and analyze the stray light: the diffraction energy of the edge of the input pupil is about 6.8 脳 10 ~ (-9) of the incident energy on the image plane, and the processing requirements of the main mirror are put forward. A set of experimental apparatus for spherical reflector corona instrument was designed and adjusted, and the optical analysis simulation model was established. The stray light level of the coronal instrument was measured by the method of point source transmittance PST curve. The validity of the simulation model is verified by comparing the distribution curves of the meridian surface on the actual image plane. Finally, the methods of calculating and measuring stray light in optical system are compared. According to the stray light coefficient and PST function formula, the stray light coefficient of the experimental device of reflective coronal apparatus is 0.278.
【學(xué)位授予單位】：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)
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2014
【分類號(hào)】：TH753.12

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